14 Herculis: Difference between revisions
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In 1998 a planet, [[14 Herculis b]] was discovered orbiting 14 Herculis via [[Doppler spectroscopy|radial velocity]].<ref name="press release"/><ref>{{cite conference|author=Mayor, M.|title=Searching for giant planets at the Haute-Provence Observatory|conference=IAU Colloqu. 170|book-title=Precise Stellar Radial Velocities|editor= Hearnshaw, J. B.|editor2= Scarfe, C. D.|date=1998|publisher=ASP|location=San Francisco|display-authors=etal}}</ref> This was formally published in 2003.<ref name="Butler2003"/> The planet has an eccentric orbit with a period of 4.8 years.<ref name="wittenmyer"/> In 2005, a possible second planet was proposed, designated [[14 Herculis c]].<ref name="Gozdziewski2006"/> The parameters of this planet were very uncertain, but an initial analysis suggested that it was in the 4:1 [[orbital resonance|resonance]] with the inner planet, with an orbital period of almost 19 years at an orbital distance of 6.9 AU.<ref name="wittenmyer"/> The existence of the planet 14 Herculis c was confirmed in 2021, along with a rough orbit determination.<ref name=Rosenthal2021/> | In 1998 a planet, [[14 Herculis b]] was discovered orbiting 14 Herculis via [[Doppler spectroscopy|radial velocity]].<ref name="press release"/><ref>{{cite conference|author=Mayor, M.|title=Searching for giant planets at the Haute-Provence Observatory|conference=IAU Colloqu. 170|book-title=Precise Stellar Radial Velocities|editor= Hearnshaw, J. B.|editor2= Scarfe, C. D.|date=1998|publisher=ASP|location=San Francisco|display-authors=etal}}</ref> This was formally published in 2003.<ref name="Butler2003"/> The planet has an eccentric orbit with a period of 4.8 years.<ref name="wittenmyer"/> In 2005, a possible second planet was proposed, designated [[14 Herculis c]].<ref name="Gozdziewski2006"/> The parameters of this planet were very uncertain, but an initial analysis suggested that it was in the 4:1 [[orbital resonance|resonance]] with the inner planet, with an orbital period of almost 19 years at an orbital distance of 6.9 AU.<ref name="wittenmyer"/> The existence of the planet 14 Herculis c was confirmed in 2021, along with a rough orbit determination.<ref name=Rosenthal2021/> | ||
A 2021 study combining radial velocity and [[astrometry]] found that the planetary orbits are not coplanar, which may indicate a strong planet-planet scattering event in the past.<ref name="Gagliuffi2021"/> Albeit one study using astrometry has found inclinations consistent with aligned orbits,<ref name="Feng2022"/> newer research including [[ | A 2021 study combining radial velocity and [[astrometry]] found that the planetary orbits are not coplanar, which may indicate a strong planet-planet scattering event in the past.<ref name="Gagliuffi2021"/> Albeit one study using astrometry has found inclinations consistent with aligned orbits,<ref name="Feng2022"/> newer research including [[James Webb Space Telescope]] observations confirm the orbits are misaligned.<ref name="Benedict2023"/><ref name="Bardalez-Gagliuffi2025"/> The planets are strongly interacting with each other. Their inclinations and eccentricities oscillate due to these gravitational interactions.<ref name="Bardalez-Gagliuffi2025"/> | ||
There are signs of a third candidate planet with a period of about 10 years, but this signal is most likely related to the star's magnetic activity cycle.<ref name="Benedict2023"/> | There are signs of a third candidate planet with a period of about 10 years, but this signal is most likely related to the star's magnetic activity cycle.<ref name="Benedict2023"/> | ||
The outer planet, 14 Herculis c, was [[direct imaging|directly imaged]] with the | The outer planet, 14 Herculis c, was [[direct imaging|directly imaged]] with the James Webb Space Telescope, re-determining its [[orbital element]]s and finding a temperature of {{convert|275|K|C|lk=in}}, among the lowest known for a directly imaged planets. Its [[apparent brightness]] is fainter than expected, hinting at [[Brown dwarf#Role of vertical mixing|disequilibrium chemistry]] and/or [[ice|water ice]] clouds.<ref name="Bardalez-Gagliuffi2025"/> | ||
{{OrbitboxPlanet begin | {{OrbitboxPlanet begin | ||
Latest revision as of 14:30, 28 June 2025
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Hercules |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | +6.61[2] |
| Characteristics | |
| Spectral type | K0 V[3] |
| B−V Template:Engvar | Template:Val[2] |
| Astrometry | |
| Radial velocity (Rv) | Template:Val[2] km/s |
| Proper motion (μ) | RA: Template:Val mas/yr[1] Dec.: Template:Val mas/yr[1] |
| Parallax (π) | 55.8657±0.0291 mas[1] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Absolute magnitude (MV) | +5.39[2] |
| Details[4] | |
| Mass | Template:Val Template:Solar mass |
| Radius | Template:Val Template:Solar radius |
| Luminosity | Template:Val[5] Template:Solar luminosity |
| Surface gravity (log g) | 4.46 cgs |
| Temperature | Template:Val K |
| Metallicity [Fe/H] | Template:Val dex |
| Rotation | 29.5 d |
| Rotational velocity (v sin i) | 1.65 km/s |
| Age | Template:Val[6] Gyr |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| Template:Odlist[7] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
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14 Herculis or 14 Her is a K-type main-sequence star Template:Convert away in the constellation Hercules. It is also known as HD 145675. Because of its apparent magnitude, of 6.61 the star can be very faintly seen with the naked eye. As of 2021, 14 Herculis is known to host two exoplanets.[4]
Stellar properties
14 Herculis is an orange dwarf star of the spectral type K0V. The star has about 98 percent of the mass, 97 percent of the radius, and only 67 percent of the luminosity of the Sun. The star appears to be 2.7 times as enriched with elements heavier than hydrogen (based on its abundance of iron), in comparison to the Sun.[4] It may have been the most metal rich star known as of 2001.[8]
Planetary system
In 1998 a planet, 14 Herculis b was discovered orbiting 14 Herculis via radial velocity.[9][10] This was formally published in 2003.[11] The planet has an eccentric orbit with a period of 4.8 years.[12] In 2005, a possible second planet was proposed, designated 14 Herculis c.[13] The parameters of this planet were very uncertain, but an initial analysis suggested that it was in the 4:1 resonance with the inner planet, with an orbital period of almost 19 years at an orbital distance of 6.9 AU.[12] The existence of the planet 14 Herculis c was confirmed in 2021, along with a rough orbit determination.[14]
A 2021 study combining radial velocity and astrometry found that the planetary orbits are not coplanar, which may indicate a strong planet-planet scattering event in the past.[4] Albeit one study using astrometry has found inclinations consistent with aligned orbits,[15] newer research including James Webb Space Telescope observations confirm the orbits are misaligned.[16][17] The planets are strongly interacting with each other. Their inclinations and eccentricities oscillate due to these gravitational interactions.[17]
There are signs of a third candidate planet with a period of about 10 years, but this signal is most likely related to the star's magnetic activity cycle.[16]
The outer planet, 14 Herculis c, was directly imaged with the James Webb Space Telescope, re-determining its orbital elements and finding a temperature of Template:Convert, among the lowest known for a directly imaged planets. Its apparent brightness is fainter than expected, hinting at disequilibrium chemistry and/or water ice clouds.[17]
Template:OrbitboxPlanet begin Template:OrbitboxPlanet Template:OrbitboxPlanet Template:Orbitbox end
See also
Notes
References
External links
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Template:14 Herculis Template:Stars of Hercules Template:Sky
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- ↑ S. Feltzing and G. Gonzalez, "The nature of super-metal-rich stars* Detailed abundance analysis of 8 super-metal-rich star candidates", 2001
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