Proxima Centauri: Difference between revisions

Proxima Centauri
	File:New shot of Proxima Centauri, our nearest neighbour.jpg; False color Hubble Space Telescope WFPC2 image taken in 2013. The bright lines are diffraction spikes.
Observation data; Epoch J2000.0 Equinox J2000.0 (ICRS)
Constellation	Centaurus
Pronunciation	Template:IPAc-en or; Template:IPAc-en
Right ascension	Template:RA
Declination	Template:DEC
Apparent magnitude (V)	10.43 – 11.11
Characteristics
Evolutionary stage	Main sequence
Spectral type	M5.5Ve
Variable type	UV Cet + BY Dra
Astrometry
Radial velocity (Rv)	Template:Val km/s
Proper motion (μ)	RA: −3781.741 mas/yr ; Dec.: 769.465 mas/yr
Parallax (π)	768.0665±0.0499 mas
Distance	Template:Rnd ± Template:Rnd ly ; (Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)	15.60
Orbit
Primary	Alpha Centauri AB
Companion	Proxima Centauri
Period (P)	Template:Val yr
Semi-major axis (a)	Template:Val
Eccentricity (e)	Template:Val
Inclination (i)	Template:Val°
Longitude of the node (Ω)	Template:Val°
Periastron epoch (T)	Template:Val
Argument of periastron (ω); (secondary)	Template:Val°
Details
Mass	Template:Val Template:Solar mass
Radius	Template:Val Template:Solar radius
Luminosity (bolometric)	0.001567±0.000020 Template:Solar luminosity
Luminosity (visual, LV)	0.00005 Template:Solar luminosity
Habitable zone inner limit	Template:Val
Habitable zone outer limit	Template:Val
Surface gravity (log g)	Template:Val cgs
Temperature	Template:Val K
Metallicity [Fe/H]	0.21 dex
Rotation	Template:Val days
Rotational velocity (v sin i)	< 0.1 km/s
Age	4.85 Gyr
Metallicity [Fe/H]	{{{metal_fe2}}} dex
Other designations
	Template:Odlist
Database references
SIMBAD	data
Exoplanet Archive	data
ARICNS	data

VisualWikitext

Latest revision as of 17:53, 18 November 2025

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Proxima Centauri, the nearest star to Earth after the Sun, is located 4.25 light-years (1.3 parsecs) away in the southern constellation of Centaurus. Discovered in 1915 by Robert Innes, it is a small, low-mass star, too faint to be seen with the naked eye, with an apparent magnitude of 11.13. Proxima Centauri is a member of the Alpha Centauri star system, being identified as component Alpha Centauri C, and is 2.18° to the southwest of the Alpha Centauri AB pair. It is currently Template:Convert from AB, which it orbits with a period of about 550,000 years. Its Latin name means the 'nearest star of Centaurus'.

Proxima Centauri is a red dwarf star with a mass about 12.5% of the Sun's mass (Template:Solar mass), and average density about 33 times that of the Sun. Because of Proxima Centauri's proximity to Earth, its angular diameter can be measured directly. Its actual diameter is about one-seventh (14%) the diameter of the Sun. Although it has a very low average luminosity, Proxima Centauri is a flare star that randomly undergoes dramatic increases in brightness because of magnetic activity. The star's magnetic field is created by convection throughout the stellar body, and the resulting flare activity generates a total X-ray emission similar to that produced by the Sun. The internal mixing of its fuel by convection through its core and Proxima's relatively low energy-production rate, mean that it will be a main-sequence star for another four trillion years.

Proxima Centauri has two known exoplanets and one candidate exoplanet: Proxima Centauri b, Proxima Centauri d and the disputed Proxima Centauri c.^{[nb 3]} Proxima Centauri b orbits the star at a distance of roughly Template:Convert with an orbital period of approximately 11.2 Earth days. Its estimated mass is at least 1.06 times that of Earth.^[8] Proxima b orbits within Proxima Centauri's habitable zone—the range where temperatures are right for liquid water to exist on its surface—but, because Proxima Centauri is a red dwarf and a flare star, the planet's habitability is highly uncertain. A sub-Earth, Proxima Centauri d, roughly Template:Convert away, orbits it every 5.1 days.^[8] A candidate sub-Neptune, Proxima Centauri c, roughly Template:Convert away from Proxima Centauri, orbits it every Template:Convert.^[16]^[17]

General characteristics

File:Relative sizes of the Alpha Centauri components and other objects (artist’s impression).tif

Relative sizes and colour of the Alpha Centauri A, B and C (Proxima) and other local stars, incl. the Sun and Jupiter for comparison (artist's impression)

File:ProxCenLightCurve.png

Three visual band light curves for Proxima Centauri are shown, illustrating the variability of Proxima. Plot A shows a superflare which dramatically increased the star's brightness for a few minutes. Plot B shows the relative brightness variation over the course of the star's 83 day rotation period. Plot C shows variation over a 6.8 year period, which may be the length of the star's magnetic activity period. Adapted from Howard et al. (2018)^[18] and Mascareño et al. (2016)^[19]

Proxima Centauri is a red dwarf, because it belongs to the main sequence on the Hertzsprung–Russell diagram and is of spectral class M5.5. The M5.5 class means that it falls in the low-mass end of M-type dwarf stars,^[14] with its hue shifted toward red-yellow^[20] by an effective temperature of Template:Val.^[9] Its absolute visual magnitude, or its visual magnitude as viewed from a distance of Template:Convert, is 15.5.^[21] Its total luminosity over all wavelengths is only 0.16% that of the Sun,^[7] although when observed in the wavelengths of visible light to which the eye is most sensitive, it is only 0.0056% as luminous as the Sun.^[22] More than 85% of its radiated power is at infrared wavelengths.^[23]

In 2002, optical interferometry with the Very Large Telescope (VLTI) found that the angular diameter of Proxima Centauri is Template:Val. Because its distance is known, the actual diameter of Proxima Centauri can be calculated to be about 1/7 that of the Sun, or 1.5 times that of Jupiter. The star's mass, estimated from stellar theory, is Template:Solar mass, or 129 Jupiter masses (Template:Jupiter mass).^[24] The mass has been calculated directly, although with less precision, from observations of microlensing events to be Template:Val.^[25]

Lower mass main-sequence stars have higher mean density than higher mass ones,^[26] and Proxima Centauri is no exception: it has a mean density of Template:Convert, compared with the Sun's mean density of Template:Convert.^{[nb 4]} The measured surface gravity of Proxima Centauri, given as the base-10 logarithm of the acceleration in units of cgs, is 5.20.^[9] This is 162 times the surface gravity on Earth.^{[nb 5]}

A 1998 study of photometric variations indicated that Proxima Centauri completes a full rotation once every 83.5 days.^[27] A subsequent time series analysis of chromospheric indicators in 2002 suggested a longer rotation period of Template:Val days.^[28] Later observations of the star's magnetic field subsequently revealed that the star rotates with a period of Template:Val days,^[29] consistent with a measurement of Template:Val days from radial velocity observations;^[30] the most recent estimate as of 2025 is Template:Val days. It is thought to rotate at an inclination of Template:Val to the line of sight.^[8]

Structure and fusion

Because of its low mass, the interior of the star is completely convective,^[31] causing energy to be transferred to the exterior by the physical movement of plasma rather than through radiative processes. This convection means that the helium ash left over from the thermonuclear fusion of hydrogen does not accumulate at the core but is instead circulated throughout the star. Unlike the Sun, which will only burn through about 10% of its total hydrogen supply before leaving the main sequence, Proxima Centauri will consume nearly all of its fuel before the fusion of hydrogen comes to an end.^[32]

Convection is associated with the generation and persistence of a magnetic field. The magnetic energy from this field is released at the surface through stellar flares that briefly (as short as per ten seconds)^[33] increase the overall luminosity of the star. On May 6, 2019, a flare event bordering Solar M and X flare class,^[34] briefly became the brightest ever detected, with a far ultraviolet emission of Template:Val.^[33] These flares can grow as large as the star and reach temperatures measured as high as 27 million K^[35]—hot enough to radiate X-rays.^[36] Proxima Centauri's quiescent X-ray luminosity, approximately (4–16)Template:E-sp erg/s ((4–16)Template:E-sp W), is roughly equal to that of the much larger Sun. The peak X-ray luminosity of the largest flares can reach Template:10^ erg/s (Template:10^ W).^[35]

Proxima Centauri's chromosphere is active, and its spectrum displays a strong emission line of singly ionized magnesium at a wavelength of 280 nm.^[37] About 88% of the surface of Proxima Centauri may be active, a percentage that is much higher than that of the Sun even at the peak of the solar cycle. Even during quiescent periods with few or no flares, this activity increases the corona temperature of Proxima Centauri to 3.5 million K, compared to the 2 million K of the Sun's corona,^[38] and its total X-ray emission is comparable to the sun's.^[39] Proxima Centauri's overall activity level is considered low compared to other red dwarfs,^[39] which is consistent with the star's estimated age of 4.85Template:E-sp years,^[14] since the activity level of a red dwarf is expected to steadily wane over billions of years as its stellar rotation rate decreases.^[40] The activity level appears to vary^[41] with a period of roughly 442 days, which is shorter than the Sun's solar cycle of 11 years.^[42]

Proxima Centauri has a relatively weak stellar wind, no more than 20% of the mass loss rate of the solar wind. Because the star is much smaller than the Sun, the mass loss per unit surface area from Proxima Centauri may be eight times that from the Sun's surface.^[43]

Life phases

File:Alpha, Beta and Proxima Centauri (1).jpg

Alpha Centauri A and B are the bright apparent star to the left, which are in a triple star system with Proxima Centauri, circled in red. The bright star system to the right is the unrelated Beta Centauri.

A red dwarf with the mass of Proxima Centauri will remain on the main sequence for about four trillion years. As the proportion of helium increases because of hydrogen fusion, the star will become smaller and hotter, gradually transforming into a so-called "blue dwarf". Near the end of this period it will become significantly more luminous, reaching 2.5% of the Sun's luminosity (Template:Solar luminosity) and warming any orbiting bodies for a period of several billion years. When the hydrogen fuel is exhausted, Proxima Centauri will then evolve into a helium white dwarf (without passing through the red giant phase) and steadily lose any remaining heat energy.^[32]^[44]

The Alpha Centauri system may have formed through a low-mass star being dynamically captured by a more massive binary of Template:Solar mass within their embedded star cluster before the cluster dispersed.^[45] However, more accurate measurements of the radial velocity are needed to confirm this hypothesis.^[46] If Proxima Centauri was bound to the Alpha Centauri system during its formation, the stars are likely to share the same elemental composition. The gravitational influence of Proxima might have disturbed the Alpha Centauri protoplanetary disks. This would have increased the delivery of volatiles such as water to the dry inner regions, so possibly enriching any terrestrial planets in the system with this material.^[46]

File:Orbital plot of Proxima Centauri.jpg

Orbital plot of Proxima Centauri around the bright apparent star Alpha Centauri AB, with position change marked (in thousands of years).

Alternatively, Proxima Centauri may have been captured at a later date during an encounter, resulting in a highly eccentric orbit that was then stabilized by the galactic tide and additional stellar encounters. Such a scenario may mean that Proxima Centauri's planetary companions have had a much lower chance for orbital disruption by Alpha Centauri.^[12] As the members of the Alpha Centauri pair continue to evolve and lose mass, Proxima Centauri is predicted to become unbound from the system in around 3.5 billion years from the present. Thereafter, the star will steadily diverge from the pair.^[47]

Motion and location

File:Angular map of fusors around Sol within 9ly (large).png

Proxima Centauri (unlabeled) next to Alpha Centauri on a radar map of all known stellar and substellar objects within 9 light years (ly), arranged clockwise in hours of right ascension, and marked by distance (▬) and position (◆)

Based on a parallax of Template:Val, published in 2020 in Gaia Data Release 3, Proxima Centauri is Template:Convert from the Sun.^[2] Previously published parallaxes include: Template:Val in 2018 by Gaia DR2, Template:Val, in 2014 by the Research Consortium On Nearby Stars;^[48] Template:Val, in the original Hipparcos Catalogue, in 1997;^[49] Template:Val in the Hipparcos New Reduction, in 2007;^[50] and Template:Val using the Hubble Space Telescope Template:'s fine guidance sensors, in 1999.^[6] From Earth's vantage point, Proxima Centauri is separated from Alpha Centauri by 2.18 degrees,^[51] or four times the angular diameter of the full Moon.^[52] Proxima Centauri has a relatively large proper motion—moving 3.85 arcseconds per year across the sky.^[53] It has a radial velocity towards the Sun of 22.2 km/s.^[5] From Proxima Centauri, the Sun would appear as a bright 0.4-magnitude star in the constellation Cassiopeia, similar to that of Achernar or Procyon from Earth.^{[nb 6]}

Among the known stars, Proxima Centauri has been the closest star to the Sun for about 32,000 years and will be so for about another 25,000 years, after which Alpha Centauri A and Alpha Centauri B will alternate approximately every 79.91 years as the closest star to the Sun. In 2001, J. García-Sánchez et al. predicted that Proxima Centauri will make its closest approach to the Sun in approximately 26,700 years, coming within Template:Convert.^[54] A 2010 study by V. V. Bobylev predicted a closest approach distance of Template:Convert in about 27,400 years,^[55] followed by a 2014 study by C. A. L. Bailer-Jones predicting a perihelion approach of Template:Convert in roughly 26,710 years.^[56] Proxima Centauri is orbiting through the Milky Way at a distance from the Galactic Centre that varies from Template:Convert, with an orbital eccentricity of 0.07.^[57]

Alpha Centauri

Script error: No such module "Labelled list hatnote". Proxima Centauri has been suspected to be a companion of the Alpha Centauri binary star system since its discovery in 1915. For this reason, it is sometimes referred to as Alpha Centauri C. Data from the Hipparcos satellite, combined with ground-based observations, were consistent with the hypothesis that the three stars are a gravitationally bound system. Kervella et al. (2017) used high-precision radial velocity measurements to determine with a high degree of confidence that Proxima and Alpha Centauri are gravitationally bound.^[5] Proxima Centauri's orbital period around the Alpha Centauri AB barycenter is Template:Val years with an eccentricity of Template:Val; it approaches Alpha Centauri to Template:Val at periastron and retreats to Template:Val at apastron.^[5] At present, Proxima Centauri is Template:Convert from the Alpha Centauri AB barycenter, nearly to the furthest point in its orbit.^[5]

Six single stars, two binary star systems, and a triple star share a common motion through space with Proxima Centauri and the Alpha Centauri system. (The co-moving stars include HD 4391, γ² Normae, and Gliese 676.) The space velocities of these stars are all within 10 km/s of Alpha Centauri's peculiar motion. Thus, they may form a moving group of stars, which would indicate a common point of origin, such as in a star cluster.^[58]

Planetary system

Template:OrbitboxPlanet begin Template:OrbitboxPlanet Template:OrbitboxPlanet Template:OrbitboxPlanet hypothetical Template:Orbitbox end

File:Proxima planetary system new.jpg

Schematic of the three planets (d, b, and c) of the Proxima Centauri system, with the habitable zone identified

As of 2025, three planets (two confirmed and one candidate) have been detected in orbit around Proxima Centauri, with one being among the lightest ever detected by radial velocity ("d"), one close to Earth's size within the habitable zone ("b"), and a possible gas dwarf that orbits much further out than the inner two ("c"), although its status remains disputed.^[8]

Searches for exoplanets around Proxima Centauri date to the late 1970s. In the 1990s, multiple measurements of Proxima Centauri's radial velocity constrained the maximum mass that a detectable companion could possess.^[6]^[59] The activity level of the star adds noise to the radial velocity measurements, complicating detection of a companion using this method.^[60] In 1998, an examination of Proxima Centauri using the Faint Object Spectrograph on board the Hubble Space Telescope appeared to show evidence of a companion orbiting at a distance of about 0.5 AU.^[61] A subsequent search using the Wide Field and Planetary Camera 2 failed to locate any companions.^[62] Astrometric measurements at the Cerro Tololo Inter-American Observatory appear to rule out a Jupiter-sized planet with an orbital period of 2−12 years.^[63]

In 2017, a team of astronomers using the Atacama Large Millimeter Array reported detecting a belt of cold dust orbiting Proxima Centauri at a range of 1−4 AU from the star. This dust has a temperature of around 40 K and has a total estimated mass of 1% of the planet Earth. They tentatively detected two additional features: a cold belt with a temperature of 10 K orbiting around 30 AU and a compact emission source about 1.2 arcseconds from the star. There was a hint at an additional warm dust belt at a distance of 0.4 AU from the star.^[64] However, upon further analysis, these emissions were determined to be most likely the result of a large flare emitted by the star in March 2017. The presence of dust within 4 AU radius from the star is not needed to model the observations.^[65]^[66]

Template:As of, radial velocity observations have ruled out the presence of any undetected planets with a minimum mass greater than Template:Earth mass with periods shorter than 10 days, Template:Earth mass in the habitable zone, Template:Earth mass up to 100 days, Template:Earth mass up to 1,000 days, and Template:Earth mass up to 10,000 days.^[8]

Planet b

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Proxima Centauri b, or Alpha Centauri Cb, orbits the star at a distance of roughly Template:Convert with an orbital period of approximately 11.2 Earth days. Its estimated mass is at least 1.07 times that of the Earth.^[67] Moreover, the equilibrium temperature of Proxima Centauri b is estimated to be within the range where water could exist as liquid on its surface; thus, placing it within the habitable zone of Proxima Centauri.^[68]^[69]^[70]

The first indications of the exoplanet Proxima Centauri b were found in 2013 by Mikko Tuomi of the University of Hertfordshire from archival observation data.^[71]^[72] To confirm the possible discovery, a team of astronomers launched the Pale Red Dot^{[nb 7]} project in January 2016. ^[73] On 24 August 2016, the team of 31 scientists from all around the world,^[74] led by Guillem Anglada-Escudé of Queen Mary University of London, confirmed the existence of Proxima Centauri b^[75] through a peer-reviewed article published in Nature.^[68]^[76] The measurements were performed using two spectrographs: HARPS on the ESO 3.6 m Telescope at La Silla Observatory and UVES on the 8 m Very Large Telescope at Paranal Observatory.^[68] Several attempts to detect a transit of this planet across the face of Proxima Centauri have been made. A transit-like signal appearing on 8 September 2016, was tentatively identified, using the Bright Star Survey Telescope at the Zhongshan Station in Antarctica.^[77]

In 2016, in a paper that helped to confirm Proxima Centauri b's existence, a second signal in the range of 60–500 days was detected. However, stellar activity and inadequate sampling causes its nature to remain unclear.^[68]

Planet c

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Proxima Centauri c is a candidate super-Earth or gas dwarf about Template:Nobr orbiting at roughly Template:Convert every Template:Convert.^[78] If Proxima Centauri b were the star's Earth, Proxima Centauri c would be equivalent to Neptune. Due to its large distance from Proxima Centauri, it is unlikely to be habitable, with a low equilibrium temperature of around 39 K.^[79] The planet was first reported by Italian astrophysicist Mario Damasso and his colleagues in April 2019.^[79]^[78] Damasso's team had noticed minor movements of Proxima Centauri in the radial velocity data from the ESO's HARPS instrument, indicating a possible additional planet orbiting Proxima Centauri.^[79] In 2020, the planet's existence was confirmed by Hubble astrometry data from Template:Circa.^[80] A possible direct imaging counterpart was detected in the infrared with the SPHERE, but the authors admit that they "did not obtain a clear detection." If their candidate source is in fact Proxima Centauri c, it is too bright for a planet of its mass and age, implying that the planet may have a ring system with a radius of around Template:Nobr However, Template:Harvp disputed the radial velocity confirmation of the planet.^[30] Template:As of, evidence for Proxima c remains inconclusive; observations with the NIRPS spectrograph were unable to confirm it, but found hints of a lower-amplitude signal with a similar period.^[8]

Planet d

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In 2019, a team of astronomers revisited the data from ESPRESSO about Proxima Centauri b to refine its mass. While doing so, the team found another radial velocity spike with a periodicity of 5.15 days. They estimated that if it were a planetary companion, it would be no less than 0.29 Earth masses.^[81] Further analysis confirmed the signal's existence leading up to the announcement of the candidate planet in February 2022.^[67] Proxima d was independently confirmed with the NIRPS spectrograph in work published in July 2025.^[8]

Habitability

Script error: No such module "Labelled list hatnote". Template:Stack Before the discovery of Proxima Centauri b, the TV documentary Alien Worlds hypothesized that a life-sustaining planet could exist in orbit around Proxima Centauri or other red dwarfs. Such a planet would lie within the habitable zone of Proxima Centauri, about Template:Convert from the star, and would have an orbital period of 3.6–14 days.^[82] A planet orbiting within this zone may experience tidal locking to the star. If the orbital eccentricity of this hypothetical planet were low, Proxima Centauri would move little in the planet's sky, and most of the surface would experience either day or night perpetually. The presence of an atmosphere could serve to redistribute heat from the star-lit side to the far side of the planet.^[83]

Proxima Centauri's flare outbursts could erode the atmosphere of any planet in its habitable zone, but the documentary's scientists thought that this obstacle could be overcome. Gibor Basri of the University of California, Berkeley argued: "No one [has] found any showstoppers to habitability." For example, one concern was that the torrents of charged particles from the star's flares could strip the atmosphere off any nearby planet. If the planet had a strong magnetic field, the field would deflect the particles from the atmosphere; even the slow rotation of a tidally locked planet that spins once for every time it orbits its star would be enough to generate a magnetic field, as long as part of the planet's interior remained molten.^[84]

Other scientists, especially proponents of the Rare Earth hypothesis,^[85] disagree that red dwarfs can sustain life. Any exoplanet in this star's habitable zone would likely be tidally locked, resulting in a relatively weak planetary magnetic moment, leading to strong atmospheric erosion by coronal mass ejections from Proxima Centauri.^[86] In December 2020, a candidate SETI radio signal BLC-1 was announced as potentially coming from the star.^[87] The signal was later determined to be human-made radio interference.^[88]

Observational history

File:ProximaCentauriLocation.png

The location of Proxima Centauri (circled in red)

In 1915, the Scottish astronomer Robert Innes, director of the Union Observatory in Johannesburg, South Africa, discovered a star that had the same proper motion as Alpha Centauri.^[89]^[90]^[91] He suggested that it be named Proxima Centauri^[92] (actually Proxima Centaurus).^[93] In 1917, at the Royal Observatory at the Cape of Good Hope, the Dutch astronomer Joan Voûte measured the star's trigonometric parallax at Template:Val and determined that Proxima Centauri was approximately the same distance from the Sun as Alpha Centauri. It was the lowest-luminosity star known at the time.^[94] An equally accurate parallax determination of Proxima Centauri was made by American astronomer Harold L. Alden in 1928, who confirmed Innes's view that it is closer, with a parallax of Template:Val.^[90]^[92]

The size of Proxima Centauri was estimated by the Canadian astronomer John Stanley Plaskett in 1925 by interferometry. The result was 207,000 miles (333,000 km), or approximately Template:Solar radius.^[95]

In 1951, American astronomer Harlow Shapley announced that Proxima Centauri is a flare star. Examination of past photographic records showed that the star displayed a measurable increase in magnitude on about 8% of the images, making it the most active flare star then known.^[96]^[97] The proximity of the star allows for detailed observation of its flare activity. In 1980, the Einstein Observatory produced a detailed X-ray energy curve of a stellar flare on Proxima Centauri. Further observations of flare activity were made with the EXOSAT and ROSAT satellites, and the X-ray emissions of smaller, solar-like flares were observed by the Japanese ASCA satellite in 1995.^[98] Proxima Centauri has since been the subject of study by most X-ray observatories, including XMM-Newton and Chandra.^[35]

Because of Proxima Centauri's southern declination, it can only be viewed south of latitude 27° N.^{[nb 8]} Red dwarfs such as Proxima Centauri are too faint to be seen with the naked eye. Even from Alpha Centauri A or B, Proxima would only be seen as a fifth magnitude star.^[99]^[100] It has apparent visual magnitude 11, so a telescope with an aperture of at least Template:Convert is needed to observe it, even under ideal viewing conditions—under clear, dark skies with Proxima Centauri well above the horizon.^[101] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars.^[102] The WGSN approved the name Proxima Centauri for this star on August 21, 2016, and it is now so included in the List of IAU approved Star Names.^[103]

In 2016, a superflare was observed from Proxima Centauri, the strongest flare ever seen. The optical brightness increased by a factor of 68× to approximately magnitude 6.8. It is estimated that similar flares occur around five times every year but are of such short duration, just a few minutes, that they had never been observed before.^[18] On 2020 April 22 and 23, the New Horizons spacecraft took images of two of the nearest stars, Proxima Centauri and Wolf 359. When compared with Earth-based images, a very large parallax effect was easily visible. However, this was only used for illustrative purposes and did not improve on previous distance measurements.^[104]^[105]

Future exploration

Script error: No such module "Labelled list hatnote". Because of the star's proximity to Earth, Proxima Centauri has been proposed as a flyby destination for interstellar travel.^[106] If non-nuclear, conventional propulsion technologies are used, the flight of a spacecraft to Proxima Centauri and its planets would probably require thousands of years.^[107] For example, Voyager 1, which is now travelling Template:Convert^[108] relative to the Sun, would reach Proxima Centauri in 73,775 years, were the spacecraft travelling in the direction of that star and Proxima was stationary. Proxima's actual galactic orbit means a slow-moving probe would have only several tens of thousands of years to catch the star at its closest approach, before it recedes out of reach.^[109]

Nuclear pulse propulsion might enable such interstellar travel with a trip timescale of a century, inspiring several studies such as Project Orion, Project Daedalus, and Project Longshot.^[109] Project Breakthrough Starshot aims to reach the Alpha Centauri system within the first half of the 21st century, with microprobes travelling at 20% of the speed of light and propelled by around 100 gigawatts of Earth-based lasers.^[110] The probes would perform a fly-by of Proxima Centauri about 20 years after its launch, or possibly go into orbit after about 140 years if swing-bys around Proxima Centauri or Alpha Centauri are to be employed.^[111] Then the probes would take photos and collect data of the planets of the stars, and their atmospheric compositions. It would take 4.25 years for the information collected to be sent back to Earth.^[112]

Explanatory notes

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References

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External links

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[78] Aron, Jacob. August 24, 2016. Proxima b: Closest Earth-like planet discovered right next door. New Scientist. Retrieved August 24, 2016

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Observation data Epoch J2000.0 Equinox J2000.0 (ICRS)
File:New shot of Proxima Centauri, our nearest neighbour.jpg False color Hubble Space Telescope WFPC2 image taken in 2013. The bright lines are diffraction spikes.
Constellation	Centaurus
Pronunciation	Template:IPAc-en or Template:IPAc-en^[1]
Right ascension	Template:RA^[2]
Declination	Template:DEC^[2]
Apparent magnitude (V)	10.43 – 11.11^[3]
Characteristics
Evolutionary stage	Main sequence
Spectral type	M5.5Ve^[4]
Variable type	UV Cet + BY Dra^[3]
Astrometry

Radial velocity (R_v)	Template:Val^[5] km/s
Proper motion (μ)	RA: −3781.741 mas/yr^[2] Dec.: 769.465 mas/yr^[2]
Parallax (π)	768.0665±0.0499 mas^[2]
Distance	Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc)
Absolute magnitude (M_V)	15.60^[6]

Orbit^[5]
Primary	Alpha Centauri AB
Companion	Proxima Centauri
Period (P)	Template:Val yr
Semi-major axis (a)	Template:Val
Eccentricity (e)	Template:Val
Inclination (i)	Template:Val°
Longitude of the node (Ω)	Template:Val°
Periastron epoch (T)	Template:Val
Argument of periastron (ω) (secondary)	Template:Val°
Details

Mass	Template:Val^[5] Template:Solar mass
Radius	Template:Val^[5] Template:Solar radius
Luminosity (bolometric)	0.001567±0.000020^[7] Template:Solar luminosity
Luminosity (visual, L_V)	0.00005^{[nb 1]} Template:Solar luminosity
Habitable zone inner limit	Template:Val^[8]
Habitable zone outer limit	Template:Val^[8]
Surface gravity (log g)	Template:Val^[9] cgs
Temperature	Template:Val^[7] K
Metallicity [Fe/H]	0.21^[10]^{[nb 2]} dex
Rotation	Template:Val^[8] days
Rotational velocity (v sin i)	< 0.1^[13] km/s
Age	4.85^[14] Gyr

Metallicity [Fe/H]	{{{metal_fe2}}} dex
Other designations
Template:Odlist^[15]
Database references
SIMBAD	data
Exoplanet Archive	data
ARICNS	data

Proxima Centauri: Difference between revisions

Latest revision as of 17:53, 18 November 2025

Contents

General characteristics

Structure and fusion

Life phases

Motion and location

Alpha Centauri

Planetary system

Planet b

Planet c

Planet d

Habitability

Observational history

Future exploration

Explanatory notes

References

Further reading

External links

Navigation menu

@@ Line 2: / Line 2: @@
 {{about|the star}}
 {{Use dmy dates|date=December 2020}}
-{{Use British English Oxford spelling|date=August 2016}}
+{{Use Oxford spelling|date=August 2016}}
 {{Featured article}}
 {{Starbox begin
@@ Line 24: / Line 24: @@
 {{Starbox character
   | type = [[Main sequence]]
-  | class = M5.5Ve<ref name=bessell>{{cite journal |bibcode=1991AJ....101..662B |title=The late-M dwarfs |journal=The Astronomical Journal |volume=101 |pages=662 |last1=Bessell |first1=M. S. |year=1991 |doi=10.1086/115714|doi-access=free }}</ref>
+  | class = M5.5Ve<ref name=bessell>{{cite journal |bibcode=1991AJ....101..662B |title=The late-M dwarfs |journal=The Astronomical Journal |volume=101 |page=662 |last1=Bessell |first1=M. S. |year=1991 |doi=10.1086/115714|doi-access=free }}</ref>
- | r-i = 2.04
+<!-- | r-i = 2.04
   | v-r = 1.68
   | b-v = 1.82
   | u-b = 1.26
   | j-h = 0.522
-  | j-k = 0.973
+  | j-k = 0.973-->
-  | variable = [[Flare star|UV Cet]] + [[BY Draconis variable|BY Dra]]<ref name=Samus_et_al_2017>{{cite journal | title=General catalogue of variable stars | version=GCVS 5.1 | last1=Samus' | first1=N. N | last2=Kazarovets | first2=E. V | last3=Durlevich | first3=O. V | last4=Kireeva | first4=N. N | last5=Pastukhova | first5=E. N | journal=Astronomy Reports | volume=61 | issue=1 | pages=80 | year=2017 | bibcode=2017ARep...61...80S | s2cid=125853869 | doi=10.1134/S1063772917010085 }}</ref>
+  | variable = [[Flare star|UV Cet]] + [[BY Draconis variable|BY Dra]]<ref name=Samus_et_al_2017>{{cite journal | title=General catalogue of variable stars | version=GCVS 5.1 | last1=Samus' | first1=N. N | last2=Kazarovets | first2=E. V | last3=Durlevich | first3=O. V | last4=Kireeva | first4=N. N | last5=Pastukhova | first5=E. N | journal=Astronomy Reports | volume=61 | issue=1 | page=80 | year=2017 | bibcode=2017ARep...61...80S | s2cid=125853869 | doi=10.1134/S1063772917010085 }}</ref>
   }}
 {{Starbox astrometry
@@ Line 40: / Line 40: @@
   | parallax = 768.0665
   | p_error = 0.0499
-  | parallax_footnote = <ref name="Gaia3">{{cite Gaia EDR3|5853498713190525696}}</ref>
+  | parallax_footnote = <ref name="Gaia3">{{cite Gaia DR3|5853498713190525696}}</ref>
   | absmag_v = 15.60<ref name="apj118"/>
   }}
@@ Line 60: / Line 60: @@
   | luminosity_bolometric = 0.001567{{±|0.000020}}<ref name="Pineda2021" />
   | luminosity_visual = 0.00005<ref group=nb>From knowing the absolute visual magnitude of Proxima Centauri, <math>M_{V_\ast} = 15.6</math>, and the absolute visual magnitude of the Sun, <math>M_{V_\odot} = 4.83</math>, the visual luminosity of Proxima Centauri can therefore be calculated: <math>L_{V_\ast}/L_{V_\odot} = 10^{0.4\left(M_{V_\odot} - M_{V_\ast}\right)} = 4.92\times10^{-5}.</math></ref>
-  | habitable_inner = <!--Inner limit to the star's habitable zone, where temperatures are 100˚ C-->
+  | habitable_inner = {{val|0.03731|0.0075|ul=au}}<ref name="SuárezMascareño2025"/>
-  | habitable_outer = <!--Outer limit to the star's habitable zone, where temperatures are 0˚ C-->
+  | habitable_outer = {{val|0.088|0.017|ul=au}}<ref name="SuárezMascareño2025"/>
   | gravity = {{val|5.20|0.23}}<ref name="aaa397" />
   | temperature = {{val|2992|49|47|fmt=commas}}<ref name="Pineda2021" />
   | metal = <!-- generally, but not by everyone, assumed to be the same as Alpha Cen A/B -->
   | metal_fe = 0.21<ref name="aaa519_A105" />{{#tag:ref|If Proxima Centauri was a later capture into the Alpha Centauri star system then its metallicity and age could be quite different to that of Alpha Centauri A and B. Through comparing Proxima Centauri to other similar stars it was estimated that it had a lower metallicity, ranging from less than a third, to about the same, of the Sun's.<ref name="PasseggerWende-von Berg2016" /><ref name="FengJones2018" />|group="nb"|name="alternate estimated metallicities"}}
-  | rotation = {{val|89.8|4}}<ref name="Klein2020">{{cite journal|title=The large-scale magnetic field of Proxima Centauri near activity maximum
+  | rotation = {{val|83.2|1.6}}<ref name="SuárezMascareño2025"/>&nbsp;days
- | last1=Klein | first1=Baptiste | last2=Donati | first2=Jean-François
- | last3=Hébrard | first3=Élodie M. | last4=Folsom | first4=Colin P.
- | last5=Morin | first5=Julien | last6=Delfosse | first6=Xavier
- | last7=Bonfils | first7=Xavier | display-authors=1
- | journal=Monthly Notices of the Royal Astronomical Society
- | volume=500 | issue=2 | pages=1844–1850
- | date=January 2021 | doi=10.1093/mnras/staa3396
- | doi-access=free | arxiv=2010.14311 | bibcode=2021MNRAS.500.1844K }}</ref>&nbsp;days
   | rotational_velocity = &lt;&nbsp;0.1<ref name="Collins2016">{{cite journal |title=Calculations of periodicity from Hα profiles of Proxima Centauri |journal=Astronomy & Astrophysics |first1=John M. |last1=Collins |first2=Hugh R. A. |last2=Jones |first3=John R. |last3=Barnes |volume=602 |at=A48 |date=June 2017 |doi=10.1051/0004-6361/201628827 |bibcode=2017A&A...602A..48C |arxiv=1608.07834|s2cid=18949162 }} See section 4: "the vsini is probably less than 0.1 km/s for Proxima Centauri".</ref>
   | age_gyr = 4.85<ref name="ESO2003" />
@@ Line 88: / Line 80: @@
 {{Starbox end}}
-'''Proxima Centauri''' is the nearest star to Earth after the [[Sun]], located 4.25 [[light-year]]s away in the southern [[constellation]] of [[Centaurus]]. This object was discovered in 1915 by [[Robert T. A. Innes|Robert Innes]]. It is a small, low-mass [[star]], too faint to be seen with the [[naked eye]], with an [[apparent magnitude]] of 11.13. Its [[Latin language|Latin]] name means the 'nearest [star] of Centaurus'. Proxima Centauri is a member of the [[Alpha Centauri]] [[star system]], being identified as component '''Alpha Centauri&nbsp;C''', and is 2.18° to the southwest of the Alpha Centauri&nbsp;AB pair. It is currently {{convert|12950|AU|ly|1|abbr=unit|lk=on}} from AB, which it orbits with a [[orbital period|period]] of about 550,000&nbsp;years.
+'''Proxima Centauri''', the nearest star to Earth after the [[Sun]], is located 4.25 [[light-year]]s (1.3 [[ parsec]]s) away in the southern [[constellation]] of [[Centaurus]]. Discovered in 1915 by [[Robert T. A. Innes|Robert Innes]], it is a small, low-mass [[star]], too faint to be seen with the [[naked eye]], with an [[apparent magnitude]] of 11.13. Proxima Centauri is a member of the [[Alpha Centauri]] [[star system]], being identified as component '''Alpha Centauri&nbsp;C''', and is 2.18° to the southwest of the Alpha Centauri&nbsp;AB pair. It is currently {{convert|12950|AU|ly|1|abbr=unit|lk=on}} from AB, which it orbits with a [[orbital period|period]] of about 550,000&nbsp;years. Its [[Latin language|Latin]] name means the 'nearest star of Centaurus'.
 Proxima Centauri is a [[red dwarf]] star with a mass about 12.5% of the Sun's mass ({{Solar mass|link=y}}), and average [[density]] about 33&nbsp;times that of the Sun. Because of Proxima Centauri's proximity to [[Earth]], its [[angular diameter]] can be measured directly. Its actual diameter is about one-seventh (14%) the diameter of the Sun. Although it has a very low average [[luminosity]], Proxima Centauri is a [[flare star]] that randomly undergoes dramatic increases in brightness because of [[magnetic activity]]. The star's [[magnetic field]] is created by [[convection]] throughout the stellar body, and the resulting flare activity generates a total [[X-ray]] emission similar to that produced by the Sun. The internal mixing of its fuel by convection through its core and Proxima's relatively low energy-production rate, mean that it will be a [[main-sequence star]] for another four trillion years.
-Proxima Centauri has one known [[exoplanet]] and two candidate exoplanets: [[Proxima Centauri b|Proxima Centauri&nbsp;b]], the candidate [[Proxima Centauri d|Proxima Centauri&nbsp;d]] and the disputed [[Proxima Centauri c|Proxima Centauri&nbsp;c]].<ref group="nb">Extrasolar planet names are designated following the [[Astronomical naming conventions#Exoplanets|International Astronomical Union's naming conventions]] in alphabetical order according to their respective dates of discovery, with 'Proxima Centauri a' being the star itself.</ref> Proxima Centauri&nbsp;b orbits the star at a distance of roughly {{convert|0.05|AU|e6km|abbr=unit}} with an orbital period of approximately 11.2 Earth days. Its estimated mass is at least 1.07&nbsp;times that of Earth.<ref name="FariaSuárezMascareñoSilva2022"/> Proxima&nbsp;b orbits within Proxima Centauri's [[habitable zone]]—the range where temperatures are right for liquid water to exist on its surface—but, because Proxima Centauri is a red dwarf and a flare star, the planet's [[Habitability of red dwarf systems|habitability]] is highly uncertain. A candidate [[super-Earth]], [[Proxima Centauri c|Proxima Centauri&nbsp;c]], roughly {{convert|1.5|AU|e6km|abbr=unit}} away from Proxima Centauri, orbits it every {{convert|1900|days|years|abbr=unit}}.<ref name="Damasso2020"/><ref name="BenedictMcArthur2020"/> A candidate [[sub-Earth]], [[Proxima Centauri d|Proxima Centauri&nbsp;d]], roughly {{convert|0.029|AU|e6km|abbr=unit}} away, orbits it every 5.1 days.<ref name="FariaSuárezMascareñoSilva2022"/>
+Proxima Centauri has two known [[exoplanet]]s and one candidate exoplanet: [[Proxima Centauri b|Proxima Centauri&nbsp;b]], [[Proxima Centauri d|Proxima Centauri&nbsp;d]] and the disputed [[Proxima Centauri c|Proxima Centauri&nbsp;c]].<ref group="nb">Extrasolar planet names are designated following the [[Astronomical naming conventions#Exoplanets|International Astronomical Union's naming conventions]] in alphabetical order according to their respective dates of discovery, with 'Proxima Centauri a' being the star itself.</ref> Proxima Centauri&nbsp;b orbits the star at a distance of roughly {{convert|0.05|AU|e6km|abbr=unit}} with an orbital period of approximately 11.2 Earth days. Its estimated mass is at least 1.06&nbsp;times that of Earth.<ref name="SuárezMascareño2025"/> Proxima&nbsp;b orbits within Proxima Centauri's [[habitable zone]]—the range where temperatures are right for liquid water to exist on its surface—but, because Proxima Centauri is a red dwarf and a flare star, the planet's [[Habitability of red dwarf systems|habitability]] is highly uncertain. A [[sub-Earth]], [[Proxima Centauri d|Proxima Centauri&nbsp;d]], roughly {{convert|0.028|AU|e6km|abbr=unit}} away, orbits it every 5.1 days.<ref name="SuárezMascareño2025"/> A candidate [[sub-Neptune]], [[Proxima Centauri c|Proxima Centauri&nbsp;c]], roughly {{convert|1.5|AU|e6km|abbr=unit}} away from Proxima Centauri, orbits it every {{convert|1900|days|years|abbr=unit}}.<ref name="Damasso2020"/><ref name="BenedictMcArthur2020"/>
 ==General characteristics==
-[[File:Relative sizes of the Alpha Centauri components and other objects (artist’s impression).tif|thumb|Relative sizes and colour of the Alpha Centauri A, B and C (Proxima) and other [[List of nearest stars and brown dwarfs|local stars]], incl. the Sun and [[Jupiter]] for comparison (artist’s impression)]][[File:ProxCenLightCurve.png|thumb|left|Three [[Photometric_system#Photometric_letters|visual band]] [[light curves]] for Proxima Centauri are shown, illustrating the variability of Proxima. Plot A shows a superflare which dramatically increased the star's brightness for a few minutes. Plot B shows the relative brightness variation over the course of the star's 83 day rotation period. Plot C shows variation over a 6.8 year period, which may be the length of the star's magnetic activity period. Adapted from Howard ''et al.'' (2018)<ref name=howard/> and Mascareño ''et al.'' (2016)<ref name="Masc2016"/>]]
+[[File:Relative sizes of the Alpha Centauri components and other objects (artist’s impression).tif|thumb|Relative sizes and colour of the Alpha Centauri A, B and C (Proxima) and other [[List of nearest stars and brown dwarfs|local stars]], incl. the Sun and [[Jupiter]] for comparison (artist's impression)]][[File:ProxCenLightCurve.png|thumb|left|Three [[Photometric system#Photometric letters|visual band]] [[light curves]] for Proxima Centauri are shown, illustrating the variability of Proxima. Plot A shows a superflare which dramatically increased the star's brightness for a few minutes. Plot B shows the relative brightness variation over the course of the star's 83 day rotation period. Plot C shows variation over a 6.8 year period, which may be the length of the star's magnetic activity period. Adapted from Howard ''et al.'' (2018)<ref name=howard/> and Mascareño ''et al.'' (2016)<ref name="Masc2016"/>]]
-Proxima Centauri is a [[red dwarf]], because it belongs to the [[main sequence]] on the [[Hertzsprung–Russell diagram]] and is of [[Stellar classification|spectral class M5.5]]. The M5.5 class means that it falls in the low-mass end of M-type [[dwarf star]]s,<ref name="ESO2003">{{cite news | last1=Kervella | first1=Pierre | last2=Thevenin | first2=Frederic |title=A family portrait of the Alpha Centauri system: VLT interferometer studies the nearest stars |publisher=European Southern Observatory |date=March 15, 2003 |url=https://www.eso.org/public/news/eso0307/ |access-date=May 10, 2016}}</ref> with its hue shifted toward red-yellow<ref>{{cite book | title=Future Spacecraft Propulsion Systems: Enabling Technologies for Space Exploration | first1=Paul A. | last1=Czysz | first2=Claudio | last2=Bruno | date=2009 | page=36 | publisher=Springer Berlin Heidelberg | isbn=9783540888147 | url=https://books.google.com/books?id=aI9QhDA4AVwC&pg=PA376 }}</ref> by an [[effective temperature]] of {{val|3000|u=K|fmt=commas|p=~}}.<ref name="aaa397" /> Its [[absolute visual magnitude]], or its visual magnitude as viewed from a distance of {{convert|10|pc|ly|0|abbr=out}}, is 15.5.<ref name="abs_mag">{{cite journal |last1=Kamper |first1=K. W. | last2=Wesselink | first2=A. J. |title=Alpha and Proxima Centauri |journal=Astronomical Journal |date=1978 |volume=83 |pages=1653–1659 |doi=10.1086/112378 |bibcode=1978AJ.....83.1653K|doi-access=free }}</ref> Its total luminosity over all [[wavelength]]s is only 0.16% that of the Sun,<ref name="Pineda2021">{{cite journal
+Proxima Centauri is a [[red dwarf]], because it belongs to the [[main sequence]] on the [[Hertzsprung–Russell diagram]] and is of [[Stellar classification|spectral class M5.5]]. The M5.5 class means that it falls in the low-mass end of M-type [[dwarf star]]s,<ref name="ESO2003">{{cite news | last1=Kervella | first1=Pierre | last2=Thevenin | first2=Frederic |title=A family portrait of the Alpha Centauri system: VLT interferometer studies the nearest stars |publisher=European Southern Observatory |date=March 15, 2003 |url=https://www.eso.org/public/news/eso0307/ |access-date=May 10, 2016}}</ref> with its hue shifted toward red-yellow<ref>{{cite book | title=Future Spacecraft Propulsion Systems: Enabling Technologies for Space Exploration | first1=Paul A. | last1=Czysz | first2=Claudio | last2=Bruno | date=2009 | page=36 | publisher=Springer Berlin Heidelberg | isbn=978-3-540-88814-7 | url=https://books.google.com/books?id=aI9QhDA4AVwC&pg=PA376 }}</ref> by an [[effective temperature]] of {{val|3000|u=K|fmt=commas|p=~}}.<ref name="aaa397" /> Its [[absolute visual magnitude]], or its visual magnitude as viewed from a distance of {{convert|10|pc|ly|0|abbr=out}}, is 15.5.<ref name="abs_mag">{{cite journal |last1=Kamper |first1=K. W. | last2=Wesselink | first2=A. J. |title=Alpha and Proxima Centauri |journal=Astronomical Journal |date=1978 |volume=83 |pages=1653–1659 |doi=10.1086/112378 |bibcode=1978AJ.....83.1653K|doi-access=free }}</ref> Its total luminosity over all [[wavelength]]s is only 0.16% that of the Sun,<ref name="Pineda2021">{{cite journal
   | title=The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars
   | last1=Pineda | first1=J. Sebastian | last2=Youngblood | first2=Allison
   | last3=France | first3=Kevin
   | journal=The Astrophysical Journal
-  | volume=918 | issue=1 | id=40 | pages=23 | date=September 2021
+  | volume=918 | issue=1 | id=40 | page=23 | date=September 2021
   | doi=10.3847/1538-4357/ac0aea | arxiv=2106.07656
   | bibcode=2021ApJ...918...40P  | s2cid=235435757 | doi-access=free }}</ref> although when observed in the wavelengths of [[visible light]] to which the eye is most sensitive, it is only 0.0056% as luminous as the Sun.<ref>{{cite book | last1=Binney | first1=James | first2=Scott | last2=Tremaine |title=Galactic dynamics |publisher=Princeton University Press |location=Princeton, New Jersey |date=1987 |isbn=978-0-691-08445-9 |page=8}}</ref> More than 85% of its radiated power is at [[infrared]] wavelengths.<ref>{{cite journal |last=Leggett |first=S. K. |title=Infrared colors of low-mass stars |journal=Astrophysical Journal Supplement Series |date=1992 |volume=82 |issue=1 |pages=351–394, 357 |doi=10.1086/191720 |bibcode=1992ApJS...82..351L}}</ref>
-In 2002, [[optical interferometry]] with the [[Very Large Telescope]] (VLTI) found that the [[angular diameter]] of Proxima Centauri is {{val|1.02|0.08|ul=mas}}. Because its distance is known, the actual diameter of Proxima Centauri can be calculated to be about 1/7 that of the Sun, or 1.5 times that of [[Jupiter]]. The star's mass, estimated from stellar theory, is {{Solar mass|12.2%|link=y}}, or 129 [[Jupiter mass]]es ({{Jupiter mass}}).<ref>{{cite web |title=How Small are Small Stars Really? |first=Didier |last=Queloz |date=November 29, 2002 |publisher=European Southern Observatory |url=https://www.eso.org/public/news/eso0232/ |access-date=September 5, 2016}}</ref> The mass has been calculated directly, although with less precision, from observations of [[microlensing]] events to be {{val|0.150|0.062|0.051|u=solar mass}}.<ref name=zurlo>{{cite journal |doi=10.1093/mnras/sty1805 |bibcode=2018MNRAS.480..236Z |title=The gravitational mass of Proxima Centauri measured with SPHERE from a microlensing event |journal=Monthly Notices of the Royal Astronomical Society |volume=480 |issue=1 |pages=236 |last1=Zurlo |first1=A. |last2=Gratton |first2=R. |last3=Mesa |first3=D. |last4=Desidera |first4=S. |last5=Enia |first5=A. |last6=Sahu |first6=K. |last7=Almenara |first7=J. -M. |last8=Kervella |first8=P. |last9=Avenhaus |first9=H.|last10=Girard|first10=J. |last11=Janson |first11=M. |last12=Lagadec |first12=E. |last13=Langlois |first13=M. |last14=Milli |first14=J. |last15=Perrot |first15=C. |last16=Schlieder |first16=J. -E. |last17=Thalmann |first17=C. |last18=Vigan |first18=A. |last19=Giro |first19=E.|last20=Gluck|first20=L. |last21=Ramos |first21=J. |last22=Roux |first22=A. |year=2018 |doi-access=free |arxiv=1807.01318|s2cid=118971274 }}</ref>
+In 2002, [[optical interferometry]] with the [[Very Large Telescope]] (VLTI) found that the [[angular diameter]] of Proxima Centauri is {{val|1.02|0.08|ul=mas}}. Because its distance is known, the actual diameter of Proxima Centauri can be calculated to be about 1/7 that of the Sun, or 1.5 times that of [[Jupiter]]. The star's mass, estimated from stellar theory, is {{Solar mass|12.2%|link=y}}, or 129 [[Jupiter mass]]es ({{Jupiter mass}}).<ref>{{cite web |title=How Small are Small Stars Really? |first=Didier |last=Queloz |date=November 29, 2002 |publisher=European Southern Observatory |url=https://www.eso.org/public/news/eso0232/ |access-date=September 5, 2016}}</ref> The mass has been calculated directly, although with less precision, from observations of [[microlensing]] events to be {{val|0.150|0.062|0.051|u=solar mass}}.<ref name=zurlo>{{cite journal |doi=10.1093/mnras/sty1805 |bibcode=2018MNRAS.480..236Z |title=The gravitational mass of Proxima Centauri measured with SPHERE from a microlensing event |journal=Monthly Notices of the Royal Astronomical Society |volume=480 |issue=1 |page=236 |last1=Zurlo |first1=A. |last2=Gratton |first2=R. |last3=Mesa |first3=D. |last4=Desidera |first4=S. |last5=Enia |first5=A. |last6=Sahu |first6=K. |last7=Almenara |first7=J. -M. |last8=Kervella |first8=P. |last9=Avenhaus |first9=H.|last10=Girard|first10=J. |last11=Janson |first11=M. |last12=Lagadec |first12=E. |last13=Langlois |first13=M. |last14=Milli |first14=J. |last15=Perrot |first15=C. |last16=Schlieder |first16=J. -E. |last17=Thalmann |first17=C. |last18=Vigan |first18=A. |last19=Giro |first19=E.|last20=Gluck|first20=L. |last21=Ramos |first21=J. |last22=Roux |first22=A. |year=2018 |doi-access=free |arxiv=1807.01318|s2cid=118971274 }}</ref>
 Lower mass main-sequence stars have higher mean [[density]] than higher mass ones,<ref>{{cite book |first=Martin V. |last=Zombeck |date=2007 |title=Handbook of space astronomy and astrophysics |url=https://archive.org/details/handbookspaceast00zomb_781 |url-access=limited |publisher=Cambridge University Press |edition=Third |pages=[https://archive.org/details/handbookspaceast00zomb_781/page/n122 109] |location=Cambridge, UK |isbn=978-0-521-78242-5}}</ref> and Proxima Centauri is no exception: it has a mean density of {{convert|47.1e3|kg/m3|g/cm3|abbr=on}}, compared with the Sun's mean density of {{convert|1.411e3|kg/m3|g/cm3|abbr=on}}.<ref group="nb" name="density">The density (''ρ'') is given by the mass divided by the volume. Relative to the Sun, therefore, the density is <math>\rho = \frac{M}{M_\odot} \cdot \left( \frac{R}{R_\odot} \right)^{-3} \cdot \rho_\odot</math> = {{nobr|0.122 · 0.154<sup>−3</sup> · (1.41{{E-sp|3}}&nbsp;kg/m<sup>3</sup>)}} = {{nobr|33.4 · (1.41{{E-sp|3}}&nbsp;kg/m<sup>3</sup>)}} = 4.71{{E-sp|4}}&nbsp;kg/m<sup>3</sup>, where <math>\rho_\odot</math> is the average solar density. See:
-* {{cite web | last1=Munsell | first1=Kirk | last2=Smith | first2=Harman | last3=Davis | first3=Phil | last4=Harvey | first4=Samantha |date=June 11, 2008 |url=http://solarsystem.nasa.gov/planets/profile.cfm?Object=Sun&Display=Facts&System=Metric |title=Sun: facts & figures |work=Solar system exploration |publisher=NASA |access-date=July 12, 2008 |url-status=dead |archive-url=https://web.archive.org/web/20080102034758/http://solarsystem.nasa.gov/planets/profile.cfm?Object=Sun&Display=Facts&System=Metric |archive-date=January 2, 2008}}
+* {{cite web | last1=Munsell | first1=Kirk | last2=Smith | first2=Harman | last3=Davis | first3=Phil | last4=Harvey | first4=Samantha |date=June 11, 2008 |url=http://solarsystem.nasa.gov/planets/profile.cfm?Object=Sun&Display=Facts&System=Metric |title=Sun: facts & figures |work=Solar system exploration |publisher=NASA |access-date=July 12, 2008 |archive-url=https://web.archive.org/web/20080102034758/http://solarsystem.nasa.gov/planets/profile.cfm?Object=Sun&Display=Facts&System=Metric |archive-date=January 2, 2008}}
 * {{cite book |last1=Bergman |first1=Marcel W. |last2=Clark |first2=T. Alan |last3=Wilson |first3=William J. F. |date=2007 |pages=220–221 |title=Observing projects using Starry Night Enthusiast |edition=8th |publisher=Macmillan |isbn=978-1-4292-0074-5}}</ref> The measured [[surface gravity]] of Proxima Centauri, given as the [[Base 10 logarithm|base-10 logarithm]] of the [[Gravitational acceleration|acceleration]] in [[cgs unit|units of cgs]], is 5.20.<ref name="aaa397" /> This is 162 times the [[Standard gravity|surface gravity]] on Earth.<ref group="nb" name="gravity">The standard surface gravity on the Earth is {{val|980.665|u=cm/s<sup>2</sup>}}, for a "log&nbsp;''g''" value of 2.992. The difference in logarithms is 5.20 − 2.99 = 2.21, yielding a multiplier of 10<sup>2.21</sup> = 162. For the Earth's gravity, see: {{cite book | page=29 | url=https://physics.nist.gov/cuu/pdf/sp330.pdf | title=The International System of Units (SI) | editor1-first=Barry N. | editor1-last=Taylor | year=2001 | publisher=United States Department of Commerce: National Institute of Standards and Technology | access-date=2012-03-08 }}</ref>
-A 1998 study of [[photometry (astronomy)|photometric]] variations indicates that Proxima Centauri completes a full rotation once every 83.5 days.<ref name=McArthur1998>{{cite journal | last1=Benedict | first1=G. F. |title=Photometry of Proxima Centauri and Barnard's Star using Hubble Space Telescope fine guidance sensor 3: a search for periodic variations |journal=The Astronomical Journal |date=1998 |volume=116 |issue=1 |pages=429–439 |doi=10.1086/300420 |bibcode=1998AJ....116..429B |arxiv=astro-ph/9806276 | last2=McArthur | first2=B. |last3=Nelan |first3=E. |last4=Story |first4=D. |last5=Whipple |first5=A. L. |last6=Shelus |first6=P. J. |last7=Jefferys |first7=W. H. |last8=Hemenway |first8=P. D. |last9=Franz |first9=Otto G.|s2cid=15880053 }}</ref> A subsequent [[time series]] analysis of [[Chromosphere|chromospheric]] indicators in 2002 suggests a longer rotation period of {{val|116.6|0.7}}&nbsp;days.<ref>{{cite journal |title=Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators |last1=Suárez Mascareño |first1=A. |last2=Rebolo |first2=R. |last3=González Hernández |first3=J. I. |last4=Esposito |first4=M. |journal=Monthly Notices of the Royal Astronomical Society |volume=452 |issue=3 |pages=2745–2756 |date=September 2015 |doi=10.1093/mnras/stv1441 |doi-access=free |bibcode=2015MNRAS.452.2745S |arxiv=1506.08039|s2cid=119181646 }}</ref> Later observations of the star's magnetic field subsequently revealed that the star rotates with a period of {{val|89.8|4}}&nbsp;days, consistent with a measurement of {{val|92.1|4.2|3.5}}&nbsp;days from radial velocity observations.<ref name="Klein2020"/><ref name="ArtigauCadieux2022"/>
+A 1998 study of [[photometry (astronomy)|photometric]] variations indicated that Proxima Centauri completes a full rotation once every 83.5 days.<ref name=McArthur1998>{{cite journal | last1=Benedict | first1=G. F. |title=Photometry of Proxima Centauri and Barnard's Star using Hubble Space Telescope fine guidance sensor 3: a search for periodic variations |journal=The Astronomical Journal |date=1998 |volume=116 |issue=1 |pages=429–439 |doi=10.1086/300420 |bibcode=1998AJ....116..429B |arxiv=astro-ph/9806276 | last2=McArthur | first2=B. |last3=Nelan |first3=E. |last4=Story |first4=D. |last5=Whipple |first5=A. L. |last6=Shelus |first6=P. J. |last7=Jefferys |first7=W. H. |last8=Hemenway |first8=P. D. |last9=Franz |first9=Otto G.|s2cid=15880053 }}</ref> A subsequent [[time series]] analysis of [[Chromosphere|chromospheric]] indicators in 2002 suggested a longer rotation period of {{val|116.6|0.7}}&nbsp;days.<ref>{{cite journal |title=Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators |last1=Suárez Mascareño |first1=A. |last2=Rebolo |first2=R. |last3=González Hernández |first3=J. I. |last4=Esposito |first4=M. |journal=Monthly Notices of the Royal Astronomical Society |volume=452 |issue=3 |pages=2745–2756 |date=September 2015 |doi=10.1093/mnras/stv1441 |doi-access=free |bibcode=2015MNRAS.452.2745S |arxiv=1506.08039|s2cid=119181646 }}</ref> Later observations of the star's magnetic field subsequently revealed that the star rotates with a period of {{val|89.8|4}}&nbsp;days,<ref name="Klein2020"/> consistent with a measurement of {{val|92.1|4.2|3.5}}&nbsp;days from radial velocity observations;<ref name="ArtigauCadieux2022"/> the most recent estimate as of 2025 is {{val|83.2|1.6}}&nbsp;days. It is thought to rotate at an [[inclination]] of {{val|47|7|u=deg}} to the line of sight.<ref name="SuárezMascareño2025"/>
 == Structure and fusion ==
-Because of its low mass, the interior of the star is completely [[Convection zone|convective]],<ref name=Yadav2016/> causing energy to be transferred to the exterior by the physical movement of plasma rather than through [[Radiation zone|radiative processes]]. This convection means that the helium ash left over from the [[thermonuclear fusion]] of hydrogen does not accumulate at the core but is instead circulated throughout the star. Unlike the Sun, which will only burn through about 10% of its total hydrogen supply before leaving the main sequence, Proxima Centauri will consume nearly all of its fuel before the fusion of hydrogen comes to an end.<ref name="adams">{{cite conference |last1=Adams |first1=Fred C. |last2=Laughlin |first2=Gregory |last3=Graves |first3=Genevieve J. M. |title=Red dwarfs and the end of the main sequence |url=http://www.astroscu.unam.mx/rmaa/RMxAC..22/PDF/RMxAC..22_adams.pdf |publisher=[[Revista Mexicana de Astronomía y Astrofísica]] |pages=46–49 |access-date=June 24, 2008 |work=Gravitational collapse: from massive stars to planets |archive-date=11 July 2019 |archive-url=https://web.archive.org/web/20190711072446/http://www.astroscu.unam.mx/rmaa/RMxAC..22/PDF/RMxAC..22_adams.pdf |url-status=dead }}</ref>
+Because of its low mass, the interior of the star is completely [[Convection zone|convective]],<ref name=Yadav2016/> causing energy to be transferred to the exterior by the physical movement of plasma rather than through [[Radiation zone|radiative processes]]. This convection means that the helium ash left over from the [[thermonuclear fusion]] of hydrogen does not accumulate at the core but is instead circulated throughout the star. Unlike the Sun, which will only burn through about 10% of its total hydrogen supply before leaving the main sequence, Proxima Centauri will consume nearly all of its fuel before the fusion of hydrogen comes to an end.<ref name="adams">{{cite conference |last1=Adams |first1=Fred C. |last2=Laughlin |first2=Gregory |last3=Graves |first3=Genevieve J. M. |title=Red dwarfs and the end of the main sequence |url=http://www.astroscu.unam.mx/rmaa/RMxAC..22/PDF/RMxAC..22_adams.pdf |publisher=[[Revista Mexicana de Astronomía y Astrofísica]] |pages=46–49 |access-date=June 24, 2008 |work=Gravitational collapse: from massive stars to planets |archive-date=11 July 2019 |archive-url=https://web.archive.org/web/20190711072446/http://www.astroscu.unam.mx/rmaa/RMxAC..22/PDF/RMxAC..22_adams.pdf }}</ref>
-Convection is associated with the generation and persistence of a [[Stellar magnetic field|magnetic field]]. The magnetic energy from this field is released at the surface through [[stellar flare]]s that briefly (as short as per ten seconds)<ref name=MacGregor_et_al_2021>{{cite journal |arxiv=2104.09519 |last1=MacGregor |first1=Meredith A. |last2=Weinberger |first2=Alycia J. |last3=Parke Loyd |first3=R. O. |last4=Shkolnik |first4=Evgenya |last5=Barclay |first5=Thomas |last6=Howard |first6=Ward S. |last7=Zic |first7=Andrew |last8=Osten |first8=Rachel A. |last9=Cranmer |first9=Steven R. |last10=Kowalski |first10=Adam F. |last11=Lenc |first11=Emil |last12=Youngblood |first12=Allison |last13=Estes |first13=Anna |last14=Wilner |first14=David J. |last15=Forbrich |first15=Jan |last16=Hughes |first16=Anna |last17=Law |first17=Nicholas M. |last18=Murphy |first18=Tara |last19=Boley |first19=Aaron |last20=Matthews |first20=Jaymie |title=Discovery of an Extremely Short Duration Flare from Proxima Centauri Using Millimeter through Far-ultraviolet Observations |journal=The Astrophysical Journal Letters |year=2021 |volume=911 |issue=2 |pages=L25 |doi=10.3847/2041-8213/abf14c |bibcode=2021ApJ...911L..25M |s2cid=233307258 |doi-access=free }}</ref> increase the overall luminosity of the star. On May 6, 2019, a flare event bordering Solar [[Solar_flare#Soft X-ray classification|M and X flare class]],<ref>{{citation|arxiv=2209.05490|year=2022|title=The Mouse That Squeaked: A Small Flare from Proxima Cen Observed in the Millimeter, Optical, and Soft X-Ray with Chandra and ALMA|doi=10.3847/1538-4357/ac9134 |last1=Howard |first1=Ward S. |last2=MacGregor |first2=Meredith A. |last3=Osten |first3=Rachel |last4=Forbrich |first4=Jan |last5=Cranmer |first5=Steven R. |last6=Tristan |first6=Isaiah |last7=Weinberger |first7=Alycia J. |last8=Youngblood |first8=Allison |last9=Barclay |first9=Thomas |last10=Parke Loyd |first10=R. O. |last11=Shkolnik |first11=Evgenya L. |last12=Zic |first12=Andrew |last13=Wilner |first13=David J. |journal=The Astrophysical Journal |volume=938 |issue=2 |page=103 |bibcode=2022ApJ...938..103H |s2cid=252211788 |doi-access=free }}</ref> briefly became the brightest ever detected, with a far ultraviolet emission of {{val|2|e=30|u=erg}}.<ref name=MacGregor_et_al_2021/> These flares can grow as large as the star and reach temperatures measured as high as 27&nbsp;million [[Kelvin|K]]<ref name=aaa416>{{cite journal |last1=Guedel |first1=M. | last2=Audard | first2=M. | last3=Reale | first3=F. | last4=Skinner | first4=S. L. | last5=Linsky | first5=J. L. |title=Flares from small to large: X-ray spectroscopy of Proxima Centauri with XMM-Newton |journal=Astronomy and Astrophysics |date=2004 |volume=416 |issue=2 |pages=713–732 |arxiv=astro-ph/0312297 |doi=10.1051/0004-6361:20031471 |bibcode=2004A&A...416..713G|s2cid=7725125 }}</ref>—hot enough to radiate [[X-ray]]s.<ref>{{cite web |url=http://chandra.harvard.edu/photo/2004/proxima/ |title=Proxima Centauri: the nearest star to the Sun |publisher=Harvard-Smithsonian Center for Astrophysics |date=August 30, 2006 |access-date=July 9, 2007}}</ref> Proxima Centauri's quiescent X-ray luminosity, approximately (4–16){{E-sp|26}}&nbsp;[[erg]]/s ((4–16){{E-sp|19}}&nbsp;[[watt|W]]), is roughly equal to that of the much larger Sun. The peak X-ray luminosity of the largest flares can reach {{10^|28}}&nbsp;erg/s ({{10^|21}}&nbsp;W).<ref name=aaa416/>
+Convection is associated with the generation and persistence of a [[Stellar magnetic field|magnetic field]]. The magnetic energy from this field is released at the surface through [[stellar flare]]s that briefly (as short as per ten seconds)<ref name=MacGregor_et_al_2021>{{cite journal |arxiv=2104.09519 |last1=MacGregor |first1=Meredith A. |last2=Weinberger |first2=Alycia J. |last3=Parke Loyd |first3=R. O. |last4=Shkolnik |first4=Evgenya |last5=Barclay |first5=Thomas |last6=Howard |first6=Ward S. |last7=Zic |first7=Andrew |last8=Osten |first8=Rachel A. |last9=Cranmer |first9=Steven R. |last10=Kowalski |first10=Adam F. |last11=Lenc |first11=Emil |last12=Youngblood |first12=Allison |last13=Estes |first13=Anna |last14=Wilner |first14=David J. |last15=Forbrich |first15=Jan |last16=Hughes |first16=Anna |last17=Law |first17=Nicholas M. |last18=Murphy |first18=Tara |last19=Boley |first19=Aaron |last20=Matthews |first20=Jaymie |title=Discovery of an Extremely Short Duration Flare from Proxima Centauri Using Millimeter through Far-ultraviolet Observations |journal=The Astrophysical Journal Letters |year=2021 |volume=911 |issue=2 |pages=L25 |doi=10.3847/2041-8213/abf14c |bibcode=2021ApJ...911L..25M |s2cid=233307258 |doi-access=free }}</ref> increase the overall luminosity of the star. On May 6, 2019, a flare event bordering Solar [[Solar flare#Soft X-ray classification|M and X flare class]],<ref>{{citation|arxiv=2209.05490|year=2022|title=The Mouse That Squeaked: A Small Flare from Proxima Cen Observed in the Millimeter, Optical, and Soft X-Ray with Chandra and ALMA|doi=10.3847/1538-4357/ac9134 |last1=Howard |first1=Ward S. |last2=MacGregor |first2=Meredith A. |last3=Osten |first3=Rachel |last4=Forbrich |first4=Jan |last5=Cranmer |first5=Steven R. |last6=Tristan |first6=Isaiah |last7=Weinberger |first7=Alycia J. |last8=Youngblood |first8=Allison |last9=Barclay |first9=Thomas |last10=Parke Loyd |first10=R. O. |last11=Shkolnik |first11=Evgenya L. |last12=Zic |first12=Andrew |last13=Wilner |first13=David J. |journal=The Astrophysical Journal |volume=938 |issue=2 |page=103 |bibcode=2022ApJ...938..103H |s2cid=252211788 |doi-access=free }}</ref> briefly became the brightest ever detected, with a far ultraviolet emission of {{val|2|e=30|u=erg}}.<ref name=MacGregor_et_al_2021/> These flares can grow as large as the star and reach temperatures measured as high as 27&nbsp;million [[Kelvin|K]]<ref name=aaa416>{{cite journal |last1=Guedel |first1=M. | last2=Audard | first2=M. | last3=Reale | first3=F. | last4=Skinner | first4=S. L. | last5=Linsky | first5=J. L. |title=Flares from small to large: X-ray spectroscopy of Proxima Centauri with XMM-Newton |journal=Astronomy and Astrophysics |date=2004 |volume=416 |issue=2 |pages=713–732 |arxiv=astro-ph/0312297 |doi=10.1051/0004-6361:20031471 |bibcode=2004A&A...416..713G|s2cid=7725125 }}</ref>—hot enough to radiate [[X-ray]]s.<ref>{{cite web |url=http://chandra.harvard.edu/photo/2004/proxima/ |title=Proxima Centauri: the nearest star to the Sun |publisher=Harvard-Smithsonian Center for Astrophysics |date=August 30, 2006 |access-date=July 9, 2007}}</ref> Proxima Centauri's quiescent X-ray luminosity, approximately (4–16){{E-sp|26}}&nbsp;[[erg]]/s ((4–16){{E-sp|19}}&nbsp;[[watt|W]]), is roughly equal to that of the much larger Sun. The peak X-ray luminosity of the largest flares can reach {{10^|28}}&nbsp;erg/s ({{10^|21}}&nbsp;W).<ref name=aaa416/>
-Proxima Centauri's [[chromosphere]] is active, and its [[stellar spectrum|spectrum]] displays a strong [[Spectral line|emission line]] of singly ionized [[magnesium]] at a wavelength of 280&nbsp;[[Nanometre|nm]].<ref>{{cite journal |first1=Guinan |last1=E. F. |last2=Morgan |first2=N. D. |title=Proxima Centauri: rotation, chromospheric activity, and flares |journal=Bulletin of the American Astronomical Society |date=1996 |volume=28 |pages=942 |bibcode=1996AAS...188.7105G}}</ref> About 88% of the surface of Proxima Centauri may be active, a percentage that is much higher than that of the Sun even at the peak of the [[solar cycle]]. Even during quiescent periods with few or no flares, this activity increases the [[stellar corona|corona]] temperature of Proxima Centauri to 3.5&nbsp;million K, compared to the 2&nbsp;million K of the Sun's corona,<ref>{{cite journal | last1=Wargelin | first1=Bradford J. | last2=Drake | first2=Jeremy J. |title=Stringent X-ray constraints on mass loss from Proxima Centauri |journal=The Astrophysical Journal |date=2002 |volume=578 |issue=1 |pages=503–514 |doi=10.1086/342270 |bibcode=2002ApJ...578..503W|doi-access=free }}</ref> and its total X-ray emission is comparable to the sun's.<ref name=apj547/> Proxima Centauri's overall activity level is considered low compared to other red dwarfs,<ref name=apj547>{{cite journal | last1=Wood | first1=B. E. | last2=Linsky | first2=J. L. | last3=Müller | first3=H.-R. | last4=Zank | first4=G. P. |title=Observational estimates for the mass-loss rates of α Centauri and Proxima Centauri using Hubble Space Telescope Lyα spectra |journal=The Astrophysical Journal |date=2001 |volume=547 |issue=1 |pages=L49–L52 |doi=10.1086/318888 |bibcode=2001ApJ...547L..49W |arxiv=astro-ph/0011153|s2cid=118537213 }}</ref> which is consistent with the star's estimated age of 4.85{{E-sp|9}}&nbsp;years,<ref name="ESO2003"/> since the activity level of a red dwarf is expected to steadily wane over billions of years as its [[stellar rotation]] rate decreases.<ref>{{cite journal |last1=Stauffer |first1=J. R. | last2=Hartmann | first2=L. W. |title=Chromospheric activity, kinematics, and metallicities of nearby M dwarfs |journal=Astrophysical Journal Supplement Series |date=1986 |volume=61 |issue=2 |pages=531–568 |bibcode=1986ApJS...61..531S |doi=10.1086/191123|doi-access=free }}</ref> The activity level appears to vary<ref>{{Cite news |last=Pulliam |first=Christine |url=http://insider.si.edu/2016/10/proxima-centauri-might-sunlike-thought/ |title=Proxima Centauri Might Be More Sunlike Than We Thought |date=October 12, 2016 |work=Smithsonian Insider |access-date=July 7, 2020}}</ref> with a period of roughly 442 days, which is shorter than the Sun's solar cycle of 11 years.<ref>{{cite journal | last1=Cincunegui | first1=C. | last2=Díaz | first2=R. F. | last3=Mauas | first3=P. J. D. |title=A possible activity cycle in Proxima Centauri |journal=Astronomy and Astrophysics |date=2007 |volume=461 |issue=3 |pages=1107–1113 |doi=10.1051/0004-6361:20066027 |bibcode=2007A&A...461.1107C |arxiv=astro-ph/0703514|s2cid=14672316 }}</ref>
+Proxima Centauri's [[chromosphere]] is active, and its [[stellar spectrum|spectrum]] displays a strong [[Spectral line|emission line]] of singly ionized [[magnesium]] at a wavelength of 280&nbsp;[[Nanometre|nm]].<ref>{{cite journal |first1=Guinan |last1=E. F. |last2=Morgan |first2=N. D. |title=Proxima Centauri: rotation, chromospheric activity, and flares |journal=Bulletin of the American Astronomical Society |date=1996 |volume=28 |page=942 |bibcode=1996AAS...188.7105G}}</ref> About 88% of the surface of Proxima Centauri may be active, a percentage that is much higher than that of the Sun even at the peak of the [[solar cycle]]. Even during quiescent periods with few or no flares, this activity increases the [[stellar corona|corona]] temperature of Proxima Centauri to 3.5&nbsp;million K, compared to the 2&nbsp;million K of the Sun's corona,<ref>{{cite journal | last1=Wargelin | first1=Bradford J. | last2=Drake | first2=Jeremy J. |title=Stringent X-ray constraints on mass loss from Proxima Centauri |journal=The Astrophysical Journal |date=2002 |volume=578 |issue=1 |pages=503–514 |doi=10.1086/342270 |bibcode=2002ApJ...578..503W|doi-access=free }}</ref> and its total X-ray emission is comparable to the sun's.<ref name=apj547/> Proxima Centauri's overall activity level is considered low compared to other red dwarfs,<ref name=apj547>{{cite journal | last1=Wood | first1=B. E. | last2=Linsky | first2=J. L. | last3=Müller | first3=H.-R. | last4=Zank | first4=G. P. |title=Observational estimates for the mass-loss rates of α Centauri and Proxima Centauri using Hubble Space Telescope Lyα spectra |journal=The Astrophysical Journal |date=2001 |volume=547 |issue=1 |pages=L49–L52 |doi=10.1086/318888 |bibcode=2001ApJ...547L..49W |arxiv=astro-ph/0011153|s2cid=118537213 }}</ref> which is consistent with the star's estimated age of 4.85{{E-sp|9}}&nbsp;years,<ref name="ESO2003"/> since the activity level of a red dwarf is expected to steadily wane over billions of years as its [[stellar rotation]] rate decreases.<ref>{{cite journal |last1=Stauffer |first1=J. R. | last2=Hartmann | first2=L. W. |title=Chromospheric activity, kinematics, and metallicities of nearby M dwarfs |journal=Astrophysical Journal Supplement Series |date=1986 |volume=61 |issue=2 |pages=531–568 |bibcode=1986ApJS...61..531S |doi=10.1086/191123|doi-access=free }}</ref> The activity level appears to vary<ref>{{Cite news |last=Pulliam |first=Christine |url=http://insider.si.edu/2016/10/proxima-centauri-might-sunlike-thought/ |title=Proxima Centauri Might Be More Sunlike Than We Thought |date=October 12, 2016 |work=Smithsonian Insider |access-date=July 7, 2020}}</ref> with a period of roughly 442 days, which is shorter than the Sun's solar cycle of 11 years.<ref>{{cite journal | last1=Cincunegui | first1=C. | last2=Díaz | first2=R. F. | last3=Mauas | first3=P. J. D. |title=A possible activity cycle in Proxima Centauri |journal=Astronomy and Astrophysics |date=2007 |volume=461 |issue=3 |pages=1107–1113 |doi=10.1051/0004-6361:20066027 |bibcode=2007A&A...461.1107C |arxiv=astro-ph/0703514|s2cid=14672316 }}</ref>
 Proxima Centauri has a relatively weak [[stellar wind]], no more than 20% of the mass loss rate of the [[solar wind]]. Because the star is much smaller than the Sun, the mass loss per unit surface area from Proxima Centauri may be eight times that from the Sun's surface.<ref>{{cite journal |last1=Wood |first1=B. E. | last2=Linsky | first2=J. L. | last3=Muller | first3=H.-R. | last4=Zank | first4=G. P. |title=Observational estimates for the mass-loss rates of Alpha Centauri and Proxima Centauri using Hubble Space Telescope Lyman-alpha spectra |journal=Astrophysical Journal |date=2000 |volume=537 |issue=2 |pages=L49–L52 |arxiv=astro-ph/0011153 |doi=10.1086/309026 |bibcode=2000ApJ...537..304W|s2cid=119332314 }}</ref>
@@ Line 134: / Line 126: @@
 [[File:Angular map of fusors around Sol within 9ly (large).png|thumb|upright=1.2| Proxima Centauri (unlabeled) next to Alpha Centauri on a radar map of all known stellar and [[substellar]] objects within 9 light years (ly), arranged clockwise in [[hour angle|hours]] of [[right ascension]], and  marked by distance (▬) and position (◆)]]
-Based on a parallax of {{val|768.0665|0.0499|u=mas}}, published in 2020 in [[Gaia Data Release 3]], Proxima Centauri is {{convert|4.2465|ly|pc AU|lk=on}} from the Sun.<ref name="Gaia3" /> Previously published parallaxes include: {{val|768.5|0.2|u=mas}} in 2018 by Gaia DR2, {{val|768.13|1.04|u=mas}}, in 2014 by the [[Research Consortium On Nearby Stars]];<ref name="lurie2014">{{cite journal |last1=Lurie |first1=John C. |last2=Henry |first2=Todd J. |last3=Jao |first3=Wei-Chun |last4=Quinn |first4=Samuel N. |last5=Winters |first5=Jennifer G. |last6=Ianna |first6=Philip A. |last7=Koerner |first7=David W. |last8=Riedel |first8=Adric R. |last9=Subasavage |first9=John P. |year=2014 |title=The Solar neighborhood. XXXIV. A search for planets orbiting nearby M dwarfs using astrometry |journal=The Astronomical Journal |volume=148 |issue=5 |pages=91 |arxiv=1407.4820 |bibcode=2014AJ....148...91L |doi=10.1088/0004-6256/148/5/91 |s2cid=118492541}}</ref> {{val|772.33|2.42|u=mas}}, in the original [[Hipparcos]] Catalogue, in 1997;<ref name="aaa323_L49">{{cite journal |last1=Perryman |first1=M. A. C. |last2=Lindegren |first2=L. |last3=Kovalevsky |first3=J. |last4=Hoeg |first4=E. |last5=Bastian |first5=U. |last6=Bernacca |first6=P. L. |last7=Crézé |first7=M. |last8=Donati |first8=F. |last9=Grenon |first9=M. |last10=Grewing |first10=M. |last11=van Leeuwen |first11=F. |date=July 1997 |title=The Hipparcos catalogue |journal=Astronomy and Astrophysics |volume=323 |pages=L49–L52 |bibcode=1997A&A...323L..49P |last12=van der Marel |first12=H. |last13=Mignard |first13=F. |last14=Murray |first14=C. A. |last15=Le Poole |first15=R. S. |last16=Schrijver |first16=H. |last17=Turon |first17=C. |last18=Arenou |first18=F. |last19=Froeschlé |first19=M. |last20=Petersen |first20=C. S.}}</ref> {{val|771.64|2.60|u=mas}} in the Hipparcos New Reduction, in 2007;<ref name="hipparcos">{{cite journal |bibcode=2007A&A...474..653V |title=Validation of the new Hipparcos reduction |journal=Astronomy and Astrophysics |volume=474 |issue=2 |pages=653–664 |last1=Van Leeuwen |first1=F. |year=2007 |doi=10.1051/0004-6361:20078357 |arxiv=0708.1752|s2cid=18759600 }}</ref> and {{val|768.77|0.37|u=mas}} using the [[Hubble Space Telescope]]{{'s}} [[fine guidance sensor]]s, in 1999.<ref name="apj118" /> From Earth's vantage point, Proxima Centauri is separated from Alpha Centauri by 2.18 degrees,<ref name="apj121">{{cite journal |last1=Kirkpatrick |first1=J. D. |last2=Davy |first2=J. |last3=Monet |first3=David G. |last4=Reid |first4=I. Neill |last5=Gizis |first5=John E. |last6=Liebert |first6=James |last7=Burgasser |first7=Adam J. |year=2001 |title=Brown dwarf companions to G-type stars. I: Gliese 417B and Gliese 584C |journal=The Astronomical Journal |volume=121 |issue=6 |pages=3235–3253 |arxiv=astro-ph/0103218 |bibcode=2001AJ....121.3235K |doi=10.1086/321085 |s2cid=18515414}}</ref> or four times the angular diameter of the full [[Moon]].<ref>{{cite web |last=Williams |first=D. R. |date=February 10, 2006 |title=Moon Fact Sheet |url=http://nssdc.gsfc.nasa.gov/planetary/factsheet/moonfact.html |access-date=October 12, 2007 |series=Lunar & Planetary Science |publisher=NASA}}</ref> Proxima Centauri has a relatively large proper motion—moving 3.85&nbsp;[[arcseconds]] per year across the sky.<ref>{{cite conference |last1=Benedict |first1=G. F. |last2=Mcarthur |first2=B. |last3=Nelan |first3=E. |last4=Story |first4=D. |last5=Jefferys |first5=W. H. |last6=Wang |first6=Q. |last7=Shelus |first7=P. J. |last8=Hemenway |first8=P. D. |last9=Mccartney |first9=J. |title=Astrometric stability and precision of fine guidance sensor #3: the parallax and proper motion of Proxima Centauri |url=http://clyde.as.utexas.edu/SpAstNEW/Papers_in_pdf/%7BBen93%7DEarlyProx.pdf |pages=380–384 |access-date=July 11, 2007 |first10=Wm. F. |last10=Van Altena |first11=R. |last11=Duncombe |first12=O. G. |last12=Franz |first13=L. W. |last13=Fredrick |work=Proceedings of the HST calibration workshop}}</ref> It has a [[radial velocity]] towards the Sun of 22.2&nbsp;km/s.<ref name="KervellaThévenin2017" /> From Proxima Centauri, the Sun would appear as a bright 0.4-magnitude star in the constellation [[Cassiopeia (constellation)|Cassiopeia]], similar to that of [[Achernar]] or [[Procyon]] from [[Earth]].<ref group="nb">The coordinates of the Sun would be diametrically opposite Proxima Centauri, at α={{RA|02|29|42.9487}}, δ={{DEC|+62|40|46.141}}. The absolute magnitude ''M<sub>v</sub>'' of the Sun is 4.83, so at a parallax ''π'' of 0.77199 the apparent magnitude ''m'' is given by 4.83 − 5(log<sub>10</sub>(0.77199) + 1) = 0.40.
+Based on a parallax of {{val|768.0665|0.0499|u=mas}}, published in 2020 in [[Gaia Data Release 3]], Proxima Centauri is {{convert|4.2465|ly|pc AU|lk=on}} from the Sun.<ref name="Gaia3" /> Previously published parallaxes include: {{val|768.5|0.2|u=mas}} in 2018 by Gaia DR2, {{val|768.13|1.04|u=mas}}, in 2014 by the [[Research Consortium On Nearby Stars]];<ref name="lurie2014">{{cite journal |last1=Lurie |first1=John C. |last2=Henry |first2=Todd J. |last3=Jao |first3=Wei-Chun |last4=Quinn |first4=Samuel N. |last5=Winters |first5=Jennifer G. |last6=Ianna |first6=Philip A. |last7=Koerner |first7=David W. |last8=Riedel |first8=Adric R. |last9=Subasavage |first9=John P. |year=2014 |title=The Solar neighborhood. XXXIV. A search for planets orbiting nearby M dwarfs using astrometry |journal=The Astronomical Journal |volume=148 |issue=5 |page=91 |arxiv=1407.4820 |bibcode=2014AJ....148...91L |doi=10.1088/0004-6256/148/5/91 |s2cid=118492541}}</ref> {{val|772.33|2.42|u=mas}}, in the original [[Hipparcos]] Catalogue, in 1997;<ref name="aaa323_L49">{{cite journal |last1=Perryman |first1=M. A. C. |last2=Lindegren |first2=L. |last3=Kovalevsky |first3=J. |last4=Hoeg |first4=E. |last5=Bastian |first5=U. |last6=Bernacca |first6=P. L. |last7=Crézé |first7=M. |last8=Donati |first8=F. |last9=Grenon |first9=M. |last10=Grewing |first10=M. |last11=van Leeuwen |first11=F. |date=July 1997 |title=The Hipparcos catalogue |journal=Astronomy and Astrophysics |volume=323 |pages=L49–L52 |bibcode=1997A&A...323L..49P |last12=van der Marel |first12=H. |last13=Mignard |first13=F. |last14=Murray |first14=C. A. |last15=Le Poole |first15=R. S. |last16=Schrijver |first16=H. |last17=Turon |first17=C. |last18=Arenou |first18=F. |last19=Froeschlé |first19=M. |last20=Petersen |first20=C. S.}}</ref> {{val|771.64|2.60|u=mas}} in the Hipparcos New Reduction, in 2007;<ref name="hipparcos">{{cite journal |bibcode=2007A&A...474..653V |title=Validation of the new Hipparcos reduction |journal=Astronomy and Astrophysics |volume=474 |issue=2 |pages=653–664 |last1=Van Leeuwen |first1=F. |year=2007 |doi=10.1051/0004-6361:20078357 |arxiv=0708.1752|s2cid=18759600 }}</ref> and {{val|768.77|0.37|u=mas}} using the [[Hubble Space Telescope]]{{'s}} [[fine guidance sensor]]s, in 1999.<ref name="apj118" /> From Earth's vantage point, Proxima Centauri is separated from Alpha Centauri by 2.18 degrees,<ref name="apj121">{{cite journal |last1=Kirkpatrick |first1=J. D. |last2=Davy |first2=J. |last3=Monet |first3=David G. |last4=Reid |first4=I. Neill |last5=Gizis |first5=John E. |last6=Liebert |first6=James |last7=Burgasser |first7=Adam J. |year=2001 |title=Brown dwarf companions to G-type stars. I: Gliese 417B and Gliese 584C |journal=The Astronomical Journal |volume=121 |issue=6 |pages=3235–3253 |arxiv=astro-ph/0103218 |bibcode=2001AJ....121.3235K |doi=10.1086/321085 |s2cid=18515414}}</ref> or four times the angular diameter of the full [[Moon]].<ref>{{cite web |last=Williams |first=D. R. |date=February 10, 2006 |title=Moon Fact Sheet |url=http://nssdc.gsfc.nasa.gov/planetary/factsheet/moonfact.html |access-date=October 12, 2007 |series=Lunar & Planetary Science |publisher=NASA}}</ref> Proxima Centauri has a relatively large proper motion—moving 3.85&nbsp;[[arcseconds]] per year across the sky.<ref>{{cite conference |last1=Benedict |first1=G. F. |last2=Mcarthur |first2=B. |last3=Nelan |first3=E. |last4=Story |first4=D. |last5=Jefferys |first5=W. H. |last6=Wang |first6=Q. |last7=Shelus |first7=P. J. |last8=Hemenway |first8=P. D. |last9=Mccartney |first9=J. |title=Astrometric stability and precision of fine guidance sensor #3: the parallax and proper motion of Proxima Centauri |url=http://clyde.as.utexas.edu/SpAstNEW/Papers_in_pdf/%7BBen93%7DEarlyProx.pdf |pages=380–384 |access-date=July 11, 2007 |first10=Wm. F. |last10=Van Altena |first11=R. |last11=Duncombe |first12=O. G. |last12=Franz |first13=L. W. |last13=Fredrick |work=Proceedings of the HST calibration workshop}}</ref> It has a [[radial velocity]] towards the Sun of 22.2&nbsp;km/s.<ref name="KervellaThévenin2017" /> From Proxima Centauri, the Sun would appear as a bright 0.4-magnitude star in the constellation [[Cassiopeia (constellation)|Cassiopeia]], similar to that of [[Achernar]] or [[Procyon]] from [[Earth]].<ref group="nb">The coordinates of the Sun would be diametrically opposite Proxima Centauri, at α={{RA|02|29|42.9487}}, δ={{DEC|+62|40|46.141}}. The absolute magnitude ''M<sub>v</sub>'' of the Sun is 4.83, so at a parallax ''π'' of 0.77199 the apparent magnitude ''m'' is given by 4.83 − 5(log<sub>10</sub>(0.77199) + 1) = 0.40.
 See: {{cite book |last=Tayler |first=Roger John |url=https://archive.org/details/starstheirstruct00tayl_311 |title=The Stars: Their Structure and Evolution |date=1994 |publisher=Cambridge University Press |isbn=978-0-521-45885-6 |page=[https://archive.org/details/starstheirstruct00tayl_311/page/n24 16] |url-access=limited}}</ref>
-Among the known stars, Proxima Centauri has been the closest star to the Sun for about 32,000&nbsp;years and will be so for about another 25,000&nbsp;years, after which Alpha Centauri A and Alpha Centauri B will alternate approximately every 79.91 years as the closest star to the Sun. In 2001, J. García-Sánchez ''et al.'' predicted that Proxima Centauri will make its closest approach to the Sun in approximately 26,700&nbsp;years, coming within {{convert|3.11|ly|pc|abbr=on}}.<ref name="aaa379">{{cite journal |last1=García-Sánchez |first1=J. |last2=Weissman |first2=P. R. |last3=Preston |first3=R. A. |last4=Jones |first4=D. L. |last5=Lestrade |first5=J.-F. |last6=Latham |first6=. W. |last7=Stefanik |first7=R. P. |last8=Paredes |first8=J. M. |date=2001 |title=Stellar encounters with the solar system |url=http://www.aanda.org/articles/aa/pdf/2001/44/aah2819.pdf |journal=Astronomy and Astrophysics |volume=379 |issue=2 |pages=634–659 |bibcode=2001A&A...379..634G |doi=10.1051/0004-6361:20011330 |doi-access=free}}</ref> A 2010 study by V. V. Bobylev predicted a closest approach distance of {{convert|2.90|ly|pc|abbr=on}} in about 27,400&nbsp;years,<ref name="al36_3_220">{{cite journal |last=Bobylev |first=V. V. |date=March 2010 |title=Searching for stars closely encountering with the solar system |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |arxiv=1003.2160 |bibcode=2010AstL...36..220B |doi=10.1134/S1063773710030060 |s2cid=118374161}}</ref> followed by a 2014 study by C. A. L. Bailer-Jones predicting a perihelion approach of {{convert|3.07|ly|pc|abbr=on}} in roughly 26,710&nbsp;years.<ref>{{cite journal |last=Bailer-Jones |first=C. A. L. |date=March 2015 |title=Close encounters of the stellar kind |journal=Astronomy & Astrophysics |volume=575 |pages=13 |arxiv=1412.3648 |bibcode=2015A&A...575A..35B |doi=10.1051/0004-6361/201425221 |id=A35 |s2cid=59039482}}</ref> Proxima Centauri is orbiting through the [[Milky Way]] at a distance from the [[Galactic Center|Galactic Centre]] that varies from {{convert|8.3|to|9.5|kpc|kly|order=flip|lk=on|abbr=on}}, with an [[orbital eccentricity]] of 0.07.<ref>{{cite journal |last1=Allen |first1=C.|author1-link=Christine Allen (astronomer) |last2=Herrera |first2=M. A. |date=1998 |title=The galactic orbits of nearby UV Ceti stars |journal=Revista Mexicana de Astronomía y Astrofísica |volume=34 |pages=37–46 |bibcode=1998RMxAA..34...37A}}</ref>
+Among the known stars, Proxima Centauri has been the closest star to the Sun for about 32,000&nbsp;years and will be so for about another 25,000&nbsp;years, after which Alpha Centauri A and Alpha Centauri B will alternate approximately every 79.91 years as the closest star to the Sun. In 2001, J. García-Sánchez ''et al.'' predicted that Proxima Centauri will make its closest approach to the Sun in approximately 26,700&nbsp;years, coming within {{convert|3.11|ly|pc|abbr=on}}.<ref name="aaa379">{{cite journal |last1=García-Sánchez |first1=J. |last2=Weissman |first2=P. R. |last3=Preston |first3=R. A. |last4=Jones |first4=D. L. |last5=Lestrade |first5=J.-F. |last6=Latham |first6=. W. |last7=Stefanik |first7=R. P. |last8=Paredes |first8=J. M. |date=2001 |title=Stellar encounters with the solar system |url=http://www.aanda.org/articles/aa/pdf/2001/44/aah2819.pdf |journal=Astronomy and Astrophysics |volume=379 |issue=2 |pages=634–659 |bibcode=2001A&A...379..634G |doi=10.1051/0004-6361:20011330 |doi-access=free}}</ref> A 2010 study by V. V. Bobylev predicted a closest approach distance of {{convert|2.90|ly|pc|abbr=on}} in about 27,400&nbsp;years,<ref name="al36_3_220">{{cite journal |last=Bobylev |first=V. V. |date=March 2010 |title=Searching for stars closely encountering with the solar system |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |arxiv=1003.2160 |bibcode=2010AstL...36..220B |doi=10.1134/S1063773710030060 |s2cid=118374161}}</ref> followed by a 2014 study by C. A. L. Bailer-Jones predicting a perihelion approach of {{convert|3.07|ly|pc|abbr=on}} in roughly 26,710&nbsp;years.<ref>{{cite journal |last=Bailer-Jones |first=C. A. L. |date=March 2015 |title=Close encounters of the stellar kind |journal=Astronomy & Astrophysics |volume=575 |page=13 |arxiv=1412.3648 |bibcode=2015A&A...575A..35B |doi=10.1051/0004-6361/201425221 |id=A35 |s2cid=59039482}}</ref> Proxima Centauri is orbiting through the [[Milky Way]] at a distance from the [[Galactic Center|Galactic Centre]] that varies from {{convert|8.3|to|9.5|kpc|kly|order=flip|lk=on|abbr=on}}, with an [[orbital eccentricity]] of 0.07.<ref>{{cite journal |last1=Allen |first1=C.|author1-link=Christine Allen (astronomer) |last2=Herrera |first2=M. A. |date=1998 |title=The galactic orbits of nearby UV Ceti stars |journal=Revista Mexicana de Astronomía y Astrofísica |volume=34 |pages=37–46 |bibcode=1998RMxAA..34...37A}}</ref>
 === Alpha Centauri ===
@@ Line 145: / Line 137: @@
 Six single stars, two binary star systems, and a triple star share a common motion through space with Proxima Centauri and the Alpha Centauri system. (The co-moving stars include [[HD 4391]], [[Gamma2 Normae|γ<sup>2</sup> Normae]], and [[Gliese 676]].) The [[space velocity (astronomy)|space velocities]] of these stars are all within 10&nbsp;km/s of Alpha Centauri's [[peculiar motion]]. Thus, they may form a [[moving group]] of stars, which would indicate a common point of origin, such as in a [[star cluster]].<ref>{{cite journal |last1=Anosova |first1=J. |last2=Orlov |first2=V. V. |last3=Pavlova |first3=N. A. |year=1994 |title=Dynamics of nearby multiple stars. The α Centauri system |journal=Astronomy and Astrophysics |volume=292 |issue=1 |pages=115–118 |bibcode=1994A&A...292..115A}}</ref>
 {{clear}}
 ==Planetary system==
 {{OrbitboxPlanet begin
 | name = Proxima Centauri
-| table_ref={{efn|<ref name=Guillem2016>
+| table_ref={{efn|Planets b & d: Suárez Mascareño et al. 2025<ref name="SuárezMascareño2025"/> (circular orbits assumed)
-{{cite journal
+<br />Planet c: Benedict & McArthur 2020;<ref name=BenedictMcArthur2020/> semi-major axis from Kervella et al. 2020<ref name=KervellaArenou2020/>
- | last1 = Anglada-Escudé    | first1  = Guillem
+<br />Predicted radii: for planet d, Faria et al. 2022;<ref name="FariaSuárezMascareñoSilva2022"/> for planet b, Brugger et al. 2016<ref name="Brugger2016">{{cite journal |last1=Brugger |first1=B. |last2=Mousis |first2=O. |last3=Deleuil |first3=M. |last4=Lunine |first4=J. I. |title=Possible Internal Structures and Compositions of Proxima Centauri b |journal=The Astrophysical Journal |date=3 November 2016 |volume=831 |issue=2 |pages=L16 |doi=10.3847/2041-8205/831/2/l16 |arxiv=1609.09757 |bibcode=2016ApJ...831L..16B |s2cid=119208249 |language=en |doi-access=free }}</ref>}}
- | last2 = Amado      | first2 = Pedro J.    | last3 = Barnes   | first3 = John
- | last4 = Berdiñas   | first4 = Zaira M.    | last5 = Butler   | first5 = R. Paul
- | last6 = Coleman    | first6  = Gavin A.L.
- | last7 = {{nobr|de la Cueva}} | first7  = Ignacio
- | last8 = Dreizler   | first8  = Stefan     | last9 = Endl     | first9 = Michael
- | last10 = Giesers   | first10 = Benjamin
- | last11 = Jeffers   | first11 = Sandra V.
- | last12 = Jenkins   | first12 = James S.
- | last13 = Jones     | first13 = Hugh R.A.
- | last14 = Kiraga    | first14 = Marcin     | last15 = Kürster | first15 = Martin
- | last16 = López-González  | first16 = María J.
- | last17 = Marvin    | first17 = Christopher J.
- | last18 = Morales   | first18 = Nicolás    | last19 = Morin   | first19 = Julien
- | last20 = Nelson    | first20 = Richard P.
- | last21 = Ortiz     | first21 = José L.    | last22 = Ofir    | first22 = Aviv
- | last23 = Paardekooper    | first23 = Sijme-Jan
- | last24 = Reiners   | first24 = Ansgar     | last25 = Rodríguez | first25 = Eloy
- | last26 = Rodríguez-López | first26 = Cristina
- | last27 = Sarmiento | first27 = Luis F.
- | last28 = Strachan  | first28 = John P.
- | last29 = Tsapras   | first29 = Yiannis    | last30 = Tuomi    | first30 = Mikko
- | last31  = Zechmeister    | first31 = Mathias
- | display-authors=6
- | year    = 2016
- | title   = A terrestrial planet candidate in a temperate orbit around Proxima Centauri
- | journal = [[Nature (journal)|Nature]]
- | volume  = 536    | issue = 7617    | pages = 437–440
- | pmid    = 27558064   | doi     = 10.1038/nature19106
- | s2cid   = 4451513    | bibcode = 2016Natur.536..437A
- | arxiv   = 1609.03449
- | url = https://www.nature.com/articles/nature19106
- | via = nature.com
 }}
-</ref><ref name=Li-2017/><ref name=Damasso2020/><ref name=KervellaArenou2020>
+{{OrbitboxPlanet
-{{cite journal
- |last1=Kervella  |first1=Pierre
- |last2=Arenou    |first2=Frédéric
- |last3=Schneider |first3=Jean
- |year=2020
- |title=Orbital inclination and mass of the exoplanet candidate Proxima&nbsp;c
- |journal=[[Astronomy & Astrophysics]]
- |volume=635 |page=L14
- |arxiv=2003.13106
- |doi=10.1051/0004-6361/202037551 |issn=0004-6361
- |bibcode= 2020A&A...635L..14K   |s2cid=214713486
-}}</ref><ref name="Suárez MascareñoFaria2020"/><ref name=BenedictMcArthur2020>
-{{cite journal
- |last1=Benedict |first1=G. Fritz
- |last2=McArthur |first2=Barbara E.
- |date=16 June 2020
- |title=A moving target: Revising the mass of Proxima Centauri&nbsp;c
- |journal=[[Research Notes of the AAS]]
- |volume=4  |issue=6  |page=86
- |doi=10.3847/2515-5172/ab9ca9 |doi-access=free
- |bibcode=2020RNAAS...4...86B |s2cid=225798015
-}}
-</ref><ref name="FariaSuárezMascareñoSilva2022"/>
-}}
-}}
-{{OrbitboxPlanet hypothetical
 | exoplanet = [[Proxima Centauri d|d]]
-| mass_earth = {{Val|0.26|0.05|p=≥}}
+| mass_earth = {{val|0.260|0.038|p=≥}}
-| period = {{Val|5.122|0.002|0.0036}}
+| period = {{val|5.12338|0.00035}}
-| semimajor = {{Val|0.02885|0.00019|0.00022}}
+| semimajor = {{val|0.02881|0.00017}}
-| radius_earth = {{Val|0.81|0.08|p=[[wiktionary:≙|≙]]}}
+| radius_earth = {{val|0.81|0.08|p=~}}{{efn|Predicted from mass-radius relationship}}
-| eccentricity = {{Val|0.04|0.15|0.04}}
+| eccentricity = 0
 | inclination =
-| status = unconfirmed{{efn|It is argued that Proxima d is confirmed because it could be detected via different methods of measuring the same radial velocity data from which Proxima&nbsp;d was discovered.<ref name="ArtigauCadieux2022"/> However, Proxima&nbsp;d is considered a candidate exoplanet by its discoverers and the [[NASA Exoplanet Archive]], because it has not been independently confirmed by more than one observatory.<ref name="Faria2022">{{cite journal |last1=Faria |first1=J. P. |last2=Suárez Mascareño |first2=A. |last3=Figueira |first3=P. |last4=Silva |first4=A. M. |last5=Damasso |first5=M. |last6=Demangeon |first6=O. |last7=Pepe |first7=F. |last8=Santos |first8=N. C. |last9=Rebolo |first9=R. |last10=Cristiani |first10=S. |last11=Adibekyan |first11=V. |display-authors=2 |date=January 4, 2022 |title=A candidate short-period sub-Earth orbiting Proxima Centauri |url=https://www.eso.org/public/archives/releases/sciencepapers/eso2202/eso2202a.pdf |journal=Astronomy & Astrophysics |publisher=European Southern Observatory |volume=658 |pages=17 |arxiv=2202.05188 |bibcode=2022A&A...658A.115F |doi=10.1051/0004-6361/202142337 |doi-access=free |last35=Tabernero |last23=Lo Curto |first18=X. |last19=Ehrenreich |first19=D. |last20=González Hernández |first20=J. I. |last21=Hara |last15=Cabral |first22=J. |first28=G. |last24=Lovis |first23=G. |first17=P. |first24=C. |last25=Martins |first25=C. J. A. P. |last26=Mégevand |first26=D. |last27=Mehner |first27=A. |last28=Micela |first21=N. |last18=Dumusque |last17=Di Marcantonio |first30=N. J. |first36=S. |last31=Pallé |first31=E. |last32=Poretti |first32=E. |last33=Sousa |first33=S. G. |last34=Sozzetti |first34=A. |last36=Udry |first15=A. |first29=P. |last37=Zapatero Osorio |first16=V. |first37=M. R. |first14=S. C. C. |last14=Barros |first13=R. |last13=Allart |first12=Y. |last12=Alibert |last30=Nunes |last29=Molaro |last16=D'Odorico |last22=Lillo-Box |first35=H.}}</ref>}}
 }}
 {{OrbitboxPlanet
 | exoplanet = [[Proxima Centauri b|b]]
-| mass_earth = ≥{{val|1.07|0.06}}
+| mass_earth = {{val|1.055|0.055|p=≥}}
-| period = {{Val|11.1868|0.0029|0.0031}}
+| period = {{val|11.18465|0.00053}}
-| semimajor = {{Val|0.04856|0.00030|0.00030}}
+| semimajor = {{val|0.04848|0.00029}}
-| radius_earth = {{Val|1.30|1.20|0.62|p=≙}}
+| radius_earth = 0.94 – 1.4{{efn|Range of possible radius values, depending on Proxima b's composition}}
-| eccentricity = {{Val|0.02|0.04|0.02}}
+| eccentricity = 0
 | inclination =
 }}
@@ Line 236: / Line 170: @@
 | radius_earth =
 | eccentricity = {{Val|0.04|0.01}}
-| inclination ={{Val|133|1}}
+| inclination = {{Val|133|1}}
-| status = disputed<ref name=ArtigauCadieux2022>
+| status = disputed<ref name=ArtigauCadieux2022/>
-{{cite journal
- |last1=Artigau   |first1=Étienne        |last2=Cadieux   |first2=Charles
- |last3=Cook      |first3=Neil J.        |last4=Doyon     |first4=René
- |last5=Vandal    |first5=Thomas         |last6=Donati    |first6=Jean-Françcois
- |last7=Moutou    |first7=Claire         |last8=Delfosse  |first8=Xavier
- |last9=Fouqué    |first9=Pascal         |last10=Martioli |first10=Eder
- |last11=Bouchy   |first11=François      |last12=Parsons  |first12=Jasmine
- |last13=Carmona  |first13=Andres        |last14=Dumusque |first14=Xavier
- |last15=Astudillo-Defru |first15=Nicola |last16=Bonfils  |first16=Xavier
- |last17=Mignon   |first17=Lucille
- |display-authors=6
- |date=23 June 2022
- |publication-date=8 August 2022
- |title=Line-by-line velocity measurements, an outlier-resistant method for precision velocimetry
- |journal=[[The Astronomical Journal]]
- |volume=164  |issue=3  |page=84
- |arxiv=2207.13524  |bibcode=2022AJ....164...84A
- |doi=10.3847/1538-3881/ac7ce6  |doi-access=free
-}}
-</ref><ref name=EPE>
-{{cite encyclopedia
- |title=Proxima Centauri&nbsp;c
- |encyclopedia=[[Extrasolar Planets Encyclopaedia]]
- |url=https://exoplanet.eu/catalog/proxima_centauri_c--7082/
- |access-date=30 July 2022
-}}
-</ref>
 }}
 {{Orbitbox end}}
 [[File:Proxima planetary system new.jpg|thumb|upright=1.2|Schematic of the three planets (d, b, and c) of the Proxima Centauri system, with the [[habitable zone]] identified]]
-As of 2022, three planets (one confirmed and two candidates) have been detected in orbit around Proxima Centauri, with one possibly being among the lightest ever detected by radial velocity ("d"), one close to Earth's size within the [[habitable zone]] ("b"), and a possible [[gas dwarf]] that orbits much further out than the inner two ("c"), although its status remains disputed.
+As of 2025, three planets (two confirmed and one candidate) have been detected in orbit around Proxima Centauri, with one being among the lightest ever detected by radial velocity ("d"), one close to Earth's size within the [[habitable zone]] ("b"), and a possible [[gas dwarf]] that orbits much further out than the inner two ("c"), although its status remains disputed.<ref name="SuárezMascareño2025"/>
 Searches for exoplanets around Proxima Centauri date to the late 1970s. In the 1990s, multiple measurements of Proxima Centauri's radial velocity constrained the maximum mass that a detectable companion could possess.<ref name=apj118>
@@ Line 307: / Line 214: @@
   | bibcode=1997ApJ...485..319S
   | url=http://pdfs.semanticscholar.org/f853/b15f7c178a7f9dd1735752d2601c6202ee63.pdf
- | url-status=dead
   | archive-url=https://web.archive.org/web/20190309110644/http://pdfs.semanticscholar.org/f853/b15f7c178a7f9dd1735752d2601c6202ee63.pdf
   | archive-date=2019-03-09
@@ Line 384: / Line 290: @@
 }}
 </ref>
+{{As of|2025}}, radial velocity observations have ruled out the presence of any undetected planets with a [[minimum mass]] greater than {{Earth mass|0.15|sym=y}} with periods shorter than 10 days, {{Earth mass|0.3|sym=y}} in the habitable zone, {{Earth mass|0.6|sym=y}} up to 100 days, {{Earth mass|1|sym=y}} up to 1,000 days, and {{Earth mass|4|sym=y}} up to 10,000 days.<ref name="SuárezMascareño2025"/>
 ===Planet b===
@@ Line 414: / Line 322: @@
   |website=Pale Red Dot
   |url=https://palereddot.org/proxima-b-is-our-closest-neighbor-better-get-used-to-it/
-  |access-date=24 August 2016 |url-status=dead
+  |access-date=24 August 2016 |archive-url=https://web.archive.org/web/20200513054609/https://palereddot.org/proxima-b-is-our-closest-neighbor-better-get-used-to-it/
- |archive-url=https://web.archive.org/web/20200513054609/https://palereddot.org/proxima-b-is-our-closest-neighbor-better-get-used-to-it/
   |archive-date=13 May 2020
 }}
@@ Line 489: / Line 396: @@
 {{main|Proxima Centauri c}}
-Proxima Centauri&nbsp;c is a candidate [[super-Earth]] or [[gas dwarf]] about {{nobr|7 {{Earth mass}}}} orbiting at roughly {{convert|1.5|AU|km}} every {{convert|1900|days|years}}.<ref name=SA-20190412/> If Proxima Centauri&nbsp;b were the star's Earth, Proxima Centauri&nbsp;c would be equivalent to Neptune. Due to its large distance from Proxima Centauri, it is unlikely to be habitable, with a low equilibrium temperature of around 39&nbsp;K.<ref name=ProximaC/> The planet was first reported by Italian astrophysicist Mario Damasso and his colleagues in April&nbsp;2019.<ref name=ProximaC>
+Proxima Centauri&nbsp;c is a candidate [[super-Earth]] or [[gas dwarf]] about {{nobr|7 {{Earth mass|sym=y}}}} orbiting at roughly {{convert|1.5|AU|km}} every {{convert|1900|days|years}}.<ref name=SA-20190412/> If Proxima Centauri&nbsp;b were the star's Earth, Proxima Centauri&nbsp;c would be equivalent to Neptune. Due to its large distance from Proxima Centauri, it is unlikely to be habitable, with a low equilibrium temperature of around 39&nbsp;K.<ref name=ProximaC/> The planet was first reported by Italian astrophysicist Mario Damasso and his colleagues in April&nbsp;2019.<ref name=ProximaC>
 {{cite news
   |first=Mike |last=Wall
@@ Line 518: / Line 425: @@
 }}
 </ref>
-A possible direct imaging counterpart was detected in the infrared with the [[Spectro-Polarimetric High-Contrast Exoplanet Research|SPHERE]], but the authors admit that they "did not obtain a clear detection." If their candidate source is in fact Proxima Centauri&nbsp;c, it is too bright for a planet of its mass and age, implying that the planet may have a [[ring system]] with a radius of around {{nobr|5 {{Jupiter radius|link=y}}.<ref name=Gratton2020/>}} However, {{harvp|Artigau|Cadieux|Cook|Doyon|Vandal|2022}} disputed the radial velocity confirmation of the planet.<ref name=ArtigauCadieux2022/>
+A possible direct imaging counterpart was detected in the infrared with the [[Spectro-Polarimetric High-Contrast Exoplanet Research|SPHERE]], but the authors admit that they "did not obtain a clear detection." If their candidate source is in fact Proxima Centauri&nbsp;c, it is too bright for a planet of its mass and age, implying that the planet may have a [[ring system]] with a radius of around {{nobr|5 {{Jupiter radius|link=y}}.<ref name=Gratton2020/>}} However, {{harvp|Artigau|Cadieux|Cook|Doyon|Vandal|2022}} disputed the radial velocity confirmation of the planet.<ref name=ArtigauCadieux2022/> {{As of|2025}}, evidence for Proxima c remains inconclusive; observations with the [[ESO 3.6 m Telescope|NIRPS]] spectrograph were unable to confirm it, but found hints of a lower-amplitude signal with a similar period.<ref name="SuárezMascareño2025"/>
 ===Planet d===
 {{main|Proxima Centauri d}}
-In 2019, a team of astronomers revisited the data from [[ESPRESSO]] about Proxima Centauri&nbsp;b to refine its mass. While doing so, the team found another radial velocity spike with a periodicity of 5.15&nbsp;days. They estimated that if it were a planetary companion, it would be no less than 0.29&nbsp;Earth masses.<ref name="Suárez MascareñoFaria2020"/> Further analysis confirmed the signal's existence leading up to the announcement of the candidate planet in February&nbsp;2022.<ref name="FariaSuárezMascareñoSilva2022"/>
+In 2019, a team of astronomers revisited the data from [[ESPRESSO]] about Proxima Centauri&nbsp;b to refine its mass. While doing so, the team found another radial velocity spike with a periodicity of 5.15&nbsp;days. They estimated that if it were a planetary companion, it would be no less than 0.29&nbsp;Earth masses.<ref name="Suárez MascareñoFaria2020"/> Further analysis confirmed the signal's existence leading up to the announcement of the candidate planet in February&nbsp;2022.<ref name="FariaSuárezMascareñoSilva2022"/> Proxima d was independently confirmed with the [[ESO 3.6 m Telescope|NIRPS]] spectrograph in work published in July 2025.<ref name="SuárezMascareño2025"/>
 ===Habitability===
@@ Line 544: / Line 451: @@
 A planet orbiting within this zone may experience [[tidal locking]] to the star. If the orbital eccentricity of this hypothetical planet were low, Proxima Centauri would move little in the planet's sky, and most of the surface would experience either day or night perpetually. The presence of an atmosphere could serve to redistribute heat from the star-lit side to the far side of the planet.<ref name="tarter">{{cite journal |title=A reappraisal of the habitability of planets around M dwarf stars |journal=[[Astrobiology (journal)|Astrobiology]] |date=2007 |volume=7 |issue=1 |pages=30–65 |doi=10.1089/ast.2006.0124 |pmid=17407403 |bibcode=2007AsBio...7...30T |arxiv=astro-ph/0609799 | last1=Tarter | first1=Jill C. | last2=Mancinelli | first2=Rocco L. | last3=Aurnou | first3=Jonathan M. | last4=Backman | first4=Dana E. | last5=Basri | first5=Gibor S. | last6=Boss | first6=Alan P. | last7=Clarke | first7=Andrew | last8=Deming | first8=Drake|s2cid=10932355 }}</ref>
-Proxima Centauri's [[Solar flare|flare]] outbursts could erode the atmosphere of any planet in its habitable zone, but the documentary's scientists thought that this obstacle could be overcome. [[Gibor Basri]] of the [[University of California, Berkeley]] argued: "No one [has] found any showstoppers to habitability." For example, one concern was that the torrents of charged particles from the star's flares could strip the atmosphere off any nearby planet. If the planet had a strong magnetic field, the field would deflect the particles from the atmosphere; even the slow rotation of a tidally locked planet that spins once for every time it orbits its star would be enough to generate a magnetic field, as long as part of the planet's interior remained molten.<ref>{{cite journal |last=Alpert |first=Mark |date=November 2005 |title=Red star rising |journal=Scientific American |volume=293 |issue=5 |pages=28 |doi=10.1038/scientificamerican1105-28 |pmid=16318021 |bibcode=2005SciAm.293e..28A}}</ref>
+Proxima Centauri's [[Solar flare|flare]] outbursts could erode the atmosphere of any planet in its habitable zone, but the documentary's scientists thought that this obstacle could be overcome. [[Gibor Basri]] of the [[University of California, Berkeley]] argued: "No one [has] found any showstoppers to habitability." For example, one concern was that the torrents of charged particles from the star's flares could strip the atmosphere off any nearby planet. If the planet had a strong magnetic field, the field would deflect the particles from the atmosphere; even the slow rotation of a tidally locked planet that spins once for every time it orbits its star would be enough to generate a magnetic field, as long as part of the planet's interior remained molten.<ref>{{cite journal |last=Alpert |first=Mark |date=November 2005 |title=Red star rising |journal=Scientific American |volume=293 |issue=5 |page=28 |doi=10.1038/scientificamerican1105-28 |pmid=16318021 |bibcode=2005SciAm.293e..28A}}</ref>
 Other scientists, especially proponents of the [[Rare Earth hypothesis]],<ref>{{cite book |first1=Peter D. |last1=Ward |author-link=Peter Ward (paleontologist) |last2=Brownlee |first2=Donald |author-link2=Donald E. Brownlee |date=2000 |title=Rare Earth: why complex life is uncommon in the universe |publisher=[[Springer Publishing]] |isbn=978-0-387-98701-9}}</ref> disagree that red dwarfs can sustain life. Any exoplanet in this star's habitable zone would likely be tidally locked, resulting in a relatively weak planetary [[magnetic moment]], leading to strong atmospheric erosion by [[coronal mass ejection]]s from Proxima Centauri.<ref name="Khodachenko">{{cite journal |title=Coronal Mass Ejection (CME) activity of low mass M stars as an important factor for the habitability of terrestrial exoplanets. I. CME impact on expected magnetospheres of earth-like exoplanets in close-in habitable zones |journal=Astrobiology |date=2007 |volume=7 |issue=1 |pages=167–184 |doi=10.1089/ast.2006.0127 |pmid=17407406 |bibcode=2007AsBio...7..167K | last1=Khodachenko | first1=Maxim L. | last2=Lammer | first2=Helmut | last3=Grießmeier | first3=Jean-Mathias | last4=Leitner | first4=Martin | last5=Selsis | first5=Franck | last6=Eiroa | first6=Carlos | last7=Hanslmeier | first7=Arnold | last8=Biernat | first8=Helfried K. }}</ref> In December 2020, a candidate [[SETI]] radio signal [[BLC-1]] was announced as potentially coming from the star.<ref name="OCallaghan2000">{{Cite web
@@ Line 561: / Line 468: @@
 [[File:ProximaCentauriLocation.png|thumb|upright=1.5|The location of Proxima Centauri (circled in red)]]In 1915, the Scottish astronomer [[Robert T. A. Innes|Robert Innes]], director of the [[Union Observatory]] in [[Johannesburg]], [[South Africa]], discovered a star that had the same [[proper motion]] as [[Alpha Centauri]].<ref name="Innes1915">{{cite journal |last1=Innes |first1=R. T. A. |date=October 1915 |title=A Faint Star of Large Proper Motion |journal=Circular of the Union Observatory Johannesburg |volume=30 |pages=235–236 |bibcode=1915CiUO...30..235I}} This is the original Proxima Centauri discovery paper.</ref><ref name="afrsky11_39">{{cite journal |last=Glass |first=I. S. |date=July 2007 |title=The discovery of the nearest star |journal=[[African Skies (journal)|African Skies]] |volume=11 |page=39 |bibcode=2007AfrSk..11...39G}}</ref><ref>{{cite web |last=Queloz |first=Didier |date=November 29, 2002 |title=How Small are Small Stars Really? |url=https://www.eso.org/public/news/eso0232/ |access-date=January 29, 2018 |publisher=European Southern Observatory |id=eso0232; PR 22/02}}</ref> He suggested that it be named ''Proxima Centauri''<ref name="aj39_913_20">{{cite journal |last=Alden |first=Harold L. |date=1928 |title=Alpha and Proxima Centauri |journal=Astronomical Journal |volume=39 |issue=913 |pages=20–23 |bibcode=1928AJ.....39...20A |doi=10.1086/104871|doi-access=free }}</ref> (actually ''Proxima Centaurus'').<ref name="Innes1917">{{cite journal |last1=Innes |first1=R. T. A. |date=September 1917 |title=Parallax of the Faint Proper Motion Star Near Alpha of Centaurus. 1900. R.A. 14{{sup|h}}22{{sup|m}}55{{sup|s}}.-0s 6t. Dec-62° 15'2 0'8 t |journal=Circular of the Union Observatory Johannesburg |volume=40 |pages=331–336 |bibcode=1917CiUO...40..331I}}</ref> In 1917, at the [[Royal Observatory, Cape of Good Hope|Royal Observatory]] at the [[Cape of Good Hope]], the Dutch astronomer [[Joan Voûte]] measured the star's trigonometric [[parallax]] at {{val|0.755|0.028|ul=″}} and determined that Proxima Centauri was approximately the same distance from the Sun as Alpha Centauri. It was the lowest-[[luminosity]] star known at the time.<ref name="Voûte1917">{{cite journal |last=Voûte |first=J. |date=1917 |title=A 13th magnitude star in Centaurus with the same parallax as α Centauri |url=https://zenodo.org/record/1431901 |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=77 |issue=9 |pages=650–651 |bibcode=1917MNRAS..77..650V |doi=10.1093/mnras/77.9.650 |doi-access=free}}</ref> An equally accurate parallax determination of Proxima Centauri was made by American astronomer [[Harold Lee Alden|Harold L. Alden]] in 1928, who confirmed Innes's view that it is closer, with a parallax of {{val|0.783|0.005|u=″}}.<ref name="afrsky11_39" /><ref name="aj39_913_20" />
-A size estimate for Proxima Centauri was obtained by the Canadian astronomer [[John Stanley Plaskett]] in 1925 using [[interferometry]]. The result was 207,000 miles (333,000 km), or approximately {{Solar radius|0.24}}.<ref>{{Cite journal |last=Plaskett |first=J. S. |date=1922 |title=The Dimensions of the Stars |url=https://www.jstor.org/stable/40668597 |journal=Publications of the Astronomical Society of the Pacific |volume=34 |issue=198 |pages=79–93 |doi=10.1086/123157 |jstor=40668597 |bibcode=1922PASP...34...79P |issn=0004-6280}}</ref>
+The size of Proxima Centauri was estimated by the Canadian astronomer [[John Stanley Plaskett]] in 1925 by [[interferometry]]. The result was 207,000 miles (333,000&nbsp;km), or approximately {{Solar radius|0.24}}.<ref>{{Cite journal |last=Plaskett |first=J. S. |date=1922 |title=The Dimensions of the Stars |journal=Publications of the Astronomical Society of the Pacific |volume=34 |issue=198 |pages=79–93 |doi=10.1086/123157 |jstor=40668597 |bibcode=1922PASP...34...79P |issn=0004-6280}}</ref>
 In 1951, American astronomer [[Harlow Shapley]] announced that Proxima Centauri is a [[flare star]]. Examination of past photographic records showed that the star displayed a measurable increase in magnitude on about 8% of the images, making it the most active flare star then known.<ref>{{cite journal |last=Shapley |first=Harlow |date=1951 |title=Proxima Centauri as a flare star |journal=Proceedings of the National Academy of Sciences of the United States of America |volume=37 |issue=1 |pages=15–18 |bibcode=1951PNAS...37...15S |doi=10.1073/pnas.37.1.15 |pmc=1063292 |pmid=16588985 |doi-access=free}}</ref><ref>{{cite journal |last1=Kroupa |first1=Pavel |last2=Burman |first2=R. R. |last3=Blair |first3=D. G. |date=1989 |title=Photometric observations of flares on Proxima Centauri |journal=PASA |volume=8 |issue=2 |pages=119–122 |bibcode=1989PASA....8..119K |doi=10.1017/S1323358000023122|s2cid=117977034 }}</ref>
@@ Line 571: / Line 478: @@
 See: {{cite book |last=Campbell |first=William Wallace |url=https://archive.org/details/elementspractic00campgoog |title=The elements of practical astronomy |date=1899 |publisher=Macmillan |location=London |pages=[https://archive.org/details/elementspractic00campgoog/page/n129 109]–110 |access-date=August 12, 2008}}</ref> Red dwarfs such as Proxima Centauri are too faint to be seen with the naked eye. Even from Alpha Centauri A or B, Proxima would only be seen as a fifth magnitude star.<ref>{{cite web |title=Proxima Centauri UV flux distribution |url=http://sdc.cab.inta-csic.es/ines/Ines_PCentre/Demos/Fluxdist/pcentauri.html |access-date=July 11, 2007 |publisher=ESA & The Astronomical Data Centre at CAB}}</ref><ref>{{cite web |last=Kaler |first=James B. |author-link=James B. Kaler |date=November 7, 2016 |title=Rigil Kentaurus |url=http://stars.astro.illinois.edu/sow/rigil-kent.html |access-date=August 3, 2008 |work=STARS |publisher=University of Illinois}}</ref> It has [[apparent visual magnitude]]&nbsp;11, so a [[telescope]] with an [[aperture]] of at least {{convert|8|cm|abbr=on}} is needed to observe it, even under ideal viewing conditions—under clear, dark skies with Proxima Centauri well above the horizon.<ref>{{cite book |last1=Sherrod |first1=P. Clay |title=A complete manual of amateur astronomy: tools and techniques for astronomical observations |last2=Koed |first2=Thomas L. |date=2003 |publisher=Courier Dover Publications |isbn=978-0-486-42820-8}}</ref> In 2016, the [[International Astronomical Union]] organized a [[IAU Working Group on Star Names|Working Group on Star Names]] (WGSN) to catalogue and standardize proper names for stars.<ref name="WGSN">{{cite web |title=IAU Working Group on Star Names (WGSN) |url=https://www.iau.org/science/scientific_bodies/working_groups/280/ |access-date=May 22, 2016 |publisher=International Astronomical Union}}</ref> The WGSN approved the name ''Proxima Centauri'' for this star on August 21, 2016, and it is now so included in the List of IAU approved Star Names.<ref name="IAU-LSN">{{cite web |title=Naming Stars |url=https://www.iau.org/public/themes/naming_stars/ |access-date=March 3, 2018 |publisher=International Astronomical Union}}</ref>
-In 2016, a [[superflare]] was observed from Proxima Centauri, the strongest flare ever seen. The optical brightness increased by a factor of 68× to approximately magnitude&nbsp;6.8. It is estimated that similar flares occur around five times every year but are of such short duration, just a few minutes, that they have never been observed before.<ref name="howard">{{cite journal |last1=Howard |first1=Ward S. |last2=Tilley |first2=Matt A. |last3=Corbett |first3=Hank |last4=Youngblood |first4=Allison |last5=Loyd |first5=R. O. Parke |last6=Ratzloff |first6=Jeffrey K. |last7=Law |first7=Nicholas M. |last8=Fors |first8=Octavi |last9=Del Ser |first9=Daniel |last10=Shkolnik |first10=Evgenya L. |last11=Ziegler |first11=Carl |year=2018 |title=The First Naked-eye Superflare Detected from Proxima Centauri |journal=The Astrophysical Journal |volume=860 |issue=2 |pages=L30 |arxiv=1804.02001 |bibcode=2018ApJ...860L..30H |doi=10.3847/2041-8213/aacaf3 |last12=Goeke |first12=Erin E. |last13=Pietraallo |first13=Aaron D. |last14=Haislip |first14=Joshua |s2cid=59127420 |doi-access=free }}</ref> On 2020 April&nbsp;22 and 23, the ''[[New Horizons]]'' spacecraft took images of two of the nearest stars, Proxima Centauri and [[Wolf 359]]. When compared with Earth-based images, a very large parallax effect was easily visible. However, this was only used for illustrative purposes and did not improve on previous distance measurements.<ref>{{cite web |date=29 January 2020 |title=Seeing Stars in 3D: The New Horizons Parallax Program |url=http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20200129 |access-date=25 May 2020 |website=pluto.jhuapl.edu |publisher=Johns Hopkins University Applied Physics Laboratory}}</ref><ref>{{cite web |title=Parallax measurements for Wolf 359 and Proxima Centauri |url=https://www.dlr.de/content/en/images/2020/3/parallax-measurements-wolf-359-and-proxima-centauri.html |access-date=19 January 2021 |website=German Aerospace Center}}</ref>
+In 2016, a [[superflare]] was observed from Proxima Centauri, the strongest flare ever seen. The optical brightness increased by a factor of 68× to approximately magnitude&nbsp;6.8. It is estimated that similar flares occur around five times every year but are of such short duration, just a few minutes, that they had never been observed before.<ref name="howard">{{cite journal |last1=Howard |first1=Ward S. |last2=Tilley |first2=Matt A. |last3=Corbett |first3=Hank |last4=Youngblood |first4=Allison |last5=Loyd |first5=R. O. Parke |last6=Ratzloff |first6=Jeffrey K. |last7=Law |first7=Nicholas M. |last8=Fors |first8=Octavi |last9=Del Ser |first9=Daniel |last10=Shkolnik |first10=Evgenya L. |last11=Ziegler |first11=Carl |year=2018 |title=The First Naked-eye Superflare Detected from Proxima Centauri |journal=The Astrophysical Journal |volume=860 |issue=2 |pages=L30 |arxiv=1804.02001 |bibcode=2018ApJ...860L..30H |doi=10.3847/2041-8213/aacaf3 |last12=Goeke |first12=Erin E. |last13=Pietraallo |first13=Aaron D. |last14=Haislip |first14=Joshua |s2cid=59127420 |doi-access=free }}</ref> On 2020 April&nbsp;22 and 23, the ''[[New Horizons]]'' spacecraft took images of two of the nearest stars, Proxima Centauri and [[Wolf 359]]. When compared with Earth-based images, a very large parallax effect was easily visible. However, this was only used for illustrative purposes and did not improve on previous distance measurements.<ref>{{cite web |date=29 January 2020 |title=Seeing Stars in 3D: The New Horizons Parallax Program |url=http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20200129 |access-date=25 May 2020 |website=pluto.jhuapl.edu |publisher=Johns Hopkins University Applied Physics Laboratory}}</ref><ref>{{cite web |title=Parallax measurements for Wolf 359 and Proxima Centauri |url=https://www.dlr.de/content/en/images/2020/3/parallax-measurements-wolf-359-and-proxima-centauri.html |access-date=19 January 2021 |website=German Aerospace Center}}</ref>
 == Future exploration ==
 {{Main|Proxima Centauri in fiction|Interstellar travel}}
-Because of the star's proximity to Earth, Proxima Centauri has been proposed as a flyby destination for interstellar travel.<ref name="gilster">{{cite book |last=Gilster |first=Paul |url=https://archive.org/details/centauridreamsim00gils |title=Centauri dreams: imagining and planning |date=2004 |publisher=Springer |isbn=978-0-387-00436-5}}</ref> If non-nuclear, conventional propulsion technologies are used, the flight of a spacecraft to Proxima Centauri and its planets would probably require thousands of years.<ref>{{cite journal |last=Crawford |first=I. A. |date=September 1990 |title=Interstellar Travel: A Review for Astronomers |journal=Quarterly Journal of the Royal Astronomical Society |volume=31 |pages=377–400 |bibcode=1990QJRAS..31..377C}}</ref> For example, ''[[Voyager 1]]'', which is now travelling {{convert|17|km/s|mph|abbr=on}}<ref>{{cite web |last=Peat |first=Chris |title=Spacecraft escaping the Solar System |url=http://www.heavens-above.com/SolarEscape.aspx |access-date=December 25, 2016 |work=Heavens Above}}</ref> relative to the Sun, would reach Proxima Centauri in 73,775 years, were the spacecraft travelling in the direction of that star and Proxima was standing still. Proxima's actual galactic orbit means a slow-moving probe would have only several tens of thousands of years to catch the star at its closest approach, before it recedes out of reach.<ref name="longshot">{{cite web |last1=Beals |first1=K. A. |last2=Beaulieu |first2=M. |last3=Dembia |first3=F. J. |last4=Kerstiens |first4=J. |last5=Kramer |first5=D. L. |last6=West |first6=J. R. |last7=Zito |first7=J. A. |date=1988 |title=Project Longshot, an Unmanned Probe to Alpha Centauri |url=https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/19890007533_1989007533.pdf |access-date=June 13, 2008 |work=NASA-CR-184718 |publisher=U. S. Naval Academy}}</ref>
+Because of the star's proximity to Earth, Proxima Centauri has been proposed as a flyby destination for interstellar travel.<ref name="gilster">{{cite book |last=Gilster |first=Paul |url=https://archive.org/details/centauridreamsim00gils |title=Centauri dreams: imagining and planning |date=2004 |publisher=Springer |isbn=978-0-387-00436-5}}</ref> If non-nuclear, conventional propulsion technologies are used, the flight of a spacecraft to Proxima Centauri and its planets would probably require thousands of years.<ref>{{cite journal |last=Crawford |first=I. A. |date=September 1990 |title=Interstellar Travel: A Review for Astronomers |journal=Quarterly Journal of the Royal Astronomical Society |volume=31 |pages=377–400 |bibcode=1990QJRAS..31..377C}}</ref> For example, ''[[Voyager 1]]'', which is now travelling {{convert|17|km/s|mph|abbr=on}}<ref>{{cite web |last=Peat |first=Chris |title=Spacecraft escaping the Solar System |url=http://www.heavens-above.com/SolarEscape.aspx |access-date=December 25, 2016 |work=Heavens Above}}</ref> relative to the Sun, would reach Proxima Centauri in 73,775 years, were the spacecraft travelling in the direction of that star and Proxima was stationary. Proxima's actual galactic orbit means a slow-moving probe would have only several tens of thousands of years to catch the star at its closest approach, before it recedes out of reach.<ref name="longshot">{{cite web |last1=Beals |first1=K. A. |last2=Beaulieu |first2=M. |last3=Dembia |first3=F. J. |last4=Kerstiens |first4=J. |last5=Kramer |first5=D. L. |last6=West |first6=J. R. |last7=Zito |first7=J. A. |date=1988 |title=Project Longshot, an Unmanned Probe to Alpha Centauri |url=https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/19890007533_1989007533.pdf |access-date=June 13, 2008 |work=NASA-CR-184718 |publisher=U. S. Naval Academy}}</ref>
-[[Nuclear pulse propulsion]] might enable such interstellar travel with a trip timescale of a century, inspiring several studies such as [[Project Orion (nuclear propulsion)|Project Orion]], [[Project Daedalus]], and [[Project Longshot]].<ref name="longshot" /> Project [[Breakthrough Starshot]] aims to reach the Alpha Centauri system within the first half of the 21st century, with microprobes travelling at 20% of the speed of light propelled by around 100 [[gigawatts]] of Earth-based lasers.<ref>{{cite journal |last=Merali |first=Zeeya |date=May 27, 2016 |title=Shooting for a star |journal=[[Science (journal)|Science]] |volume=352 |issue=6289 |pages=1040–1041 |doi=10.1126/science.352.6289.1040 |pmid=27230357}}</ref> The probes would perform a fly-by of Proxima Centauri about 20 years after its launch, or possibly go into orbit after about 140 years if [[swing-by]]'s around Proxima Centauri or Alpha Centauri are to be employed.<ref name="Heller Hippke 2023 k319">{{cite web | last1=Heller | first1=René | last2=Hippke | first2=Michael | title=Full braking at Alpha Centauri | website=Max-Planck-Gesellschaft | date=July 11, 2023 | url=https://www.mpg.de/11019256/full-braking-at-alpha-centauri | access-date=December 3, 2023}}</ref> Then the probes would take photos and collect data of the planets of the stars, and their atmospheric compositions. It would take 4.25 years for the information collected to be sent back to Earth.<ref name="Popkin2017">{{cite journal |last=Popkin |first=Gabriel |date=February 2, 2017 |title=What it would take to reach the stars |journal=[[Nature (journal)|Nature]] |volume=542 |issue=7639 |pages=20–22 |bibcode=2017Natur.542...20P |doi=10.1038/542020a |pmid=28150784 |doi-access=free}}</ref>
+[[Nuclear pulse propulsion]] might enable such interstellar travel with a trip timescale of a century, inspiring several studies such as [[Project Orion (nuclear propulsion)|Project Orion]], [[Project Daedalus]], and [[Project Longshot]].<ref name="longshot" /> Project [[Breakthrough Starshot]] aims to reach the Alpha Centauri system within the first half of the 21st century, with microprobes travelling at 20% of the speed of light and propelled by around 100 [[gigawatts]] of Earth-based lasers.<ref>{{cite journal |last=Merali |first=Zeeya |date=May 27, 2016 |title=Shooting for a star |journal=[[Science (journal)|Science]] |volume=352 |issue=6289 |pages=1040–1041 |doi=10.1126/science.352.6289.1040 |pmid=27230357}}</ref> The probes would perform a fly-by of Proxima Centauri about 20 years after its launch, or possibly go into orbit after about 140 years if [[swing-by]]s around Proxima Centauri or Alpha Centauri are to be employed.<ref name="Heller Hippke 2023 k319">{{cite web | last1=Heller | first1=René | last2=Hippke | first2=Michael | title=Full braking at Alpha Centauri | website=Max-Planck-Gesellschaft | date=July 11, 2023 | url=https://www.mpg.de/11019256/full-braking-at-alpha-centauri | access-date=December 3, 2023}}</ref> Then the probes would take photos and collect data of the planets of the stars, and their atmospheric compositions. It would take 4.25 years for the information collected to be sent back to Earth.<ref name="Popkin2017">{{cite journal |last=Popkin |first=Gabriel |date=February 2, 2017 |title=What it would take to reach the stars |journal=[[Nature (journal)|Nature]] |volume=542 |issue=7639 |pages=20–22 |bibcode=2017Natur.542...20P |doi=10.1038/542020a |pmid=28150784 |doi-access=free}}</ref>
 == Explanatory notes==
@@ Line 680: / Line 587: @@
   |last11=Adibekyan  |first11=V.          |last12=Alibert    |first12=Y.
   |last13=Allart     |first13=R.          |last14=Barros     |first14=S.C.C.
-  |last15=Cabral     |first15=A.          |last16=D’Odorico  |first16=V.
+  |last15=Cabral     |first15=A.          |last16=D'Odorico  |first16=V.
   |last17=di&nbsp;Marcantonio |first17=P.
   |last18=Dumusque   |first18=X.          |last19=Ehrenreich |first19=D.
@@ Line 701: / Line 608: @@
   |arxiv=2202.05188  |bibcode=2022A&A...658A.115F
   |url=https://www.eso.org/public/archives/releases/sciencepapers/eso2202/eso2202a.pdf
-  |via=eso.org
+  |via=eso.org <!-- |publisher=EDP Sciences -->
-<!-- |publisher=EDP Sciences -->
 }}
 </ref>
@@ Line 738: / Line 644: @@
   | doi=10.1051/0004-6361/202037594  | s2cid = 215754278
   | bibcode= 2020A&A...638A.120G  | arxiv = 2004.06685
-}}
-</ref>
-<ref name=Li-2017>
-{{cite journal
- |last1=Li        |first1=Yiting   |last2=Stefansson |first2=Gudmundur
- |last3=Robertson |first3=Paul     |last4=Monson     |first4=Andrew
- |last5=Cañas     |first5=Caleb
- |last6=Mahadevan |first6=Suvrath  |author6-link=Suvrath Mahadevan
- |name-list-style=amp
- |date=14 December 2017
- |title=A candidate transit event around Proxima Centauri
- |journal=[[Research Notes of the AAS]]
- |volume=1  |issue=1  |page=49
- |doi=10.3847/2515-5172/aaa0d5  |doi-access=free
- |arxiv=1712.04483  |s2cid=119034883
- |bibcode=2017RNAAS...1...49L
 }}
 </ref>
@@ Line 826: / Line 715: @@
 }}
 </ref>
+<ref name=Guillem2016>
+{{cite journal
+ | last1 = Anglada-Escudé    | first1  = Guillem
+ | last2 = Amado      | first2 = Pedro J.    | last3 = Barnes   | first3 = John
+ | last4 = Berdiñas   | first4 = Zaira M.    | last5 = Butler   | first5 = R. Paul
+ | last6 = Coleman    | first6  = Gavin A.L.
+ | last7 = {{nobr|de la Cueva}} | first7  = Ignacio
+ | last8 = Dreizler   | first8  = Stefan     | last9 = Endl     | first9 = Michael
+ | last10 = Giesers   | first10 = Benjamin
+ | last11 = Jeffers   | first11 = Sandra V.
+ | last12 = Jenkins   | first12 = James S.
+ | last13 = Jones     | first13 = Hugh R.A.
+ | last14 = Kiraga    | first14 = Marcin     | last15 = Kürster | first15 = Martin
+ | last16 = López-González  | first16 = María J.
+ | last17 = Marvin    | first17 = Christopher J.
+ | last18 = Morales   | first18 = Nicolás    | last19 = Morin   | first19 = Julien
+ | last20 = Nelson    | first20 = Richard P.
+ | last21 = Ortiz     | first21 = José L.    | last22 = Ofir    | first22 = Aviv
+ | last23 = Paardekooper    | first23 = Sijme-Jan
+ | last24 = Reiners   | first24 = Ansgar     | last25 = Rodríguez | first25 = Eloy
+ | last26 = Rodríguez-López | first26 = Cristina
+ | last27 = Sarmiento | first27 = Luis F.
+ | last28 = Strachan  | first28 = John P.
+ | last29 = Tsapras   | first29 = Yiannis    | last30 = Tuomi    | first30 = Mikko
+ | last31  = Zechmeister    | first31 = Mathias
+ | display-authors=6
+ | year    = 2016
+ | title   = A terrestrial planet candidate in a temperate orbit around Proxima Centauri
+ | journal = [[Nature (journal)|Nature]]
+ | volume  = 536    | issue = 7617    | pages = 437–440
+ | pmid    = 27558064   | doi     = 10.1038/nature19106
+ | s2cid   = 4451513    | bibcode = 2016Natur.536..437A
+ | arxiv   = 1609.03449
+ | url = https://www.nature.com/articles/nature19106
+ | via = nature.com
+}}
+</ref>
+<ref name=KervellaArenou2020>
+{{cite journal
+ |last1=Kervella  |first1=Pierre
+ |last2=Arenou    |first2=Frédéric
+ |last3=Schneider |first3=Jean
+ |year=2020
+ |title=Orbital inclination and mass of the exoplanet candidate Proxima&nbsp;c
+ |journal=[[Astronomy & Astrophysics]]
+ |volume=635 |page=L14
+ |arxiv=2003.13106
+ |doi=10.1051/0004-6361/202037551 |issn=0004-6361
+ |bibcode= 2020A&A...635L..14K   |s2cid=214713486
+}}</ref>
+<ref name=BenedictMcArthur2020>
+{{cite journal
+ |last1=Benedict |first1=G. Fritz
+ |last2=McArthur |first2=Barbara E.
+ |date=16 June 2020
+ |title=A moving target: Revising the mass of Proxima Centauri&nbsp;c
+ |journal=[[Research Notes of the AAS]]
+ |volume=4  |issue=6  |page=86
+ |doi=10.3847/2515-5172/ab9ca9 |doi-access=free
+ |bibcode=2020RNAAS...4...86B |s2cid=225798015
+}}
+</ref>
+<ref name="Klein2020">{{cite journal|title=The large-scale magnetic field of Proxima Centauri near activity maximum
+ | last1=Klein | first1=Baptiste | last2=Donati | first2=Jean-François
+ | last3=Hébrard | first3=Élodie M. | last4=Folsom | first4=Colin P.
+ | last5=Morin | first5=Julien | last6=Delfosse | first6=Xavier
+ | last7=Bonfils | first7=Xavier | display-authors=1
+ | journal=Monthly Notices of the Royal Astronomical Society
+ | volume=500 | issue=2 | pages=1844–1850
+ | date=January 2021 | doi=10.1093/mnras/staa3396
+ | doi-access=free | arxiv=2010.14311 | bibcode=2021MNRAS.500.1844K }}</ref>
+<ref name=ArtigauCadieux2022>
+{{cite journal
+ |last1=Artigau   |first1=Étienne        |last2=Cadieux   |first2=Charles
+ |last3=Cook      |first3=Neil J.        |last4=Doyon     |first4=René
+ |last5=Vandal    |first5=Thomas         |last6=Donati    |first6=Jean-Françcois
+ |last7=Moutou    |first7=Claire         |last8=Delfosse  |first8=Xavier
+ |last9=Fouqué    |first9=Pascal         |last10=Martioli |first10=Eder
+ |last11=Bouchy   |first11=François      |last12=Parsons  |first12=Jasmine
+ |last13=Carmona  |first13=Andres        |last14=Dumusque |first14=Xavier
+ |last15=Astudillo-Defru |first15=Nicola |last16=Bonfils  |first16=Xavier
+ |last17=Mignon   |first17=Lucille
+ |display-authors=6
+ |date=23 June 2022
+ |publication-date=8 August 2022
+ |title=Line-by-line velocity measurements, an outlier-resistant method for precision velocimetry
+ |journal=[[The Astronomical Journal]]
+ |volume=164  |issue=3  |page=84
+ |arxiv=2207.13524  |bibcode=2022AJ....164...84A
+ |doi=10.3847/1538-3881/ac7ce6  |doi-access=free
+}}
+</ref>
+<ref name="SuárezMascareño2025">
+{{cite journal
+ | last1=Suárez Mascareño | first1=Alejandro | last2=Artigau | first2=Étienne | display-authors=etal
+ | date=29 July 2025
+ | title=Diving into the planetary system of Proxima with NIRPS: Breaking the metre per second barrier in the infrared
+ | journal=[[Astronomy & Astrophysics]]
+ | volume=700 | issue= |pages=A11
+ | arxiv=2507.21751
+ | doi=10.1051/0004-6361/202553728 | bibcode=2025A&A...700A..11S | doi-access=free
+}}</ref>
 }} <!-- end "refs=" -->
@@ Line 1,013: / Line 1,010: @@
 * {{cite web |url=http://www.southastrodel.com/PageAlphaCen006.htm |title=Voyage to Alpha Centauri |series=The Imperial Star – Alpha Centauri |publisher=Southern Astronomical Delights |last=James |first=Andrew |date=March 11, 2008 |access-date=August 5, 2008}}
 * {{cite web |url=http://www.solstation.com/stars/alp-cent3.htm |title=Alpha Centauri 3 |work=SolStation |access-date=August 5, 2008}}
-* {{cite web |url=http://www.uranometrianova.pro.br/astronomia/AA002/alphacen.htm |title=O Sistema Alpha Centauri |access-date=June 25, 2008 |work=Astronomia & Astrofísica |language=pt |archive-date=3 March 2016 |archive-url=https://web.archive.org/web/20160303190444/http://www.uranometrianova.pro.br/astronomia/AA002/alphacen.htm |url-status=dead }}
+* {{cite web |url=http://www.uranometrianova.pro.br/astronomia/AA002/alphacen.htm |title=O Sistema Alpha Centauri |access-date=June 25, 2008 |work=Astronomia & Astrofísica |language=pt |archive-date=3 March 2016 |archive-url=https://web.archive.org/web/20160303190444/http://www.uranometrianova.pro.br/astronomia/AA002/alphacen.htm }}
 * {{cite web |url=http://www.wikisky.org/?ra=14.495264&de=-62.67948000000001&zoom=8&show_grid=1&show_constellation_lines=1&show_constellation_boundaries=1&show_const_names=0&show_galaxies=1&show_box=1&box_ra=14.495264&box_de=-62.67948&box_width=50&box_height=50&img_source=DSS2 |title=Image of Proxima Centauri |work=Wikisky |access-date=July 1, 2017}}
 * {{cite web |url=http://www.constellation-guide.com/proxima-centauri/ |title=Proxima Centauri |website=Constellation-guide.com |access-date=August 25, 2016}}
@@ Line 1,024: / Line 1,021: @@
 {{Stars of Centaurus}}
 {{Portal bar|Astronomy|Stars|Spaceflight|Outer space}}
+<!-- Properties -->
 {{DEFAULTSORT:Proxima Centauri}}
-<!-- Properties -->
 [[Category:Proxima Centauri| ]]
 [[Category:M-type main-sequence stars]]