14 Herculis: Difference between revisions

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{{Starbox reference
{{Starbox reference
| Simbad = HD+145675
| Simbad = HD+145675
| NSTED = HD-145675
}}
}}
{{Starbox end}}
{{Starbox end}}


'''14 Herculis''' or '''14 Her''' is a [[K-type main-sequence star]] {{convert|58.4|ly|pc|lk=on|abbr=off}} away in the [[constellation]] [[Hercules (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 [[exoplanet]]s in orbit around the star.<ref name="Gagliuffi2021"/>
'''14 Herculis''' or '''14 Her''' is a [[K-type main-sequence star]] {{convert|58.4|ly|pc|lk=on|abbr=off}} away in the [[constellation]] [[Hercules (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 [[exoplanet]]s.<ref name="Gagliuffi2021"/>


== Stellar properties ==
== Stellar properties ==
Line 54: Line 55:
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"/> Subsequent astrometric studies have found differing results; a 2022 study found inclinations consistent with aligned orbits,<ref name="Feng2022"/> while a 2023 study again found misaligned orbits.<ref name="Benedict2023"/> The latter study also found 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"/>
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"/>


Direct imaging of the outer planet 14 Herculis c with the [[James Webb Space Telescope]] is planned.<ref>{{cite web |url=https://www.stsci.edu/jwst/science-execution/program-information.html?id=3337 |title=Solving a Solar Neighborhood Crime Scene by Imaging 14 Her c |publisher=[[Space Telescope Science Institute|STScI]] |access-date=29 May 2023}}</ref>
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 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
| table_ref = <ref name="Gagliuffi2021"/><ref name="Benedict2023"/>
| table_ref = {{efn|1=Inclinations: Xiao
''et al.'' (2025)<ref name=Xiao2025/><br>14 Her b mass, axis and period: Feng ''et al.'' (2024)<ref name=Feng2024/><br>14 Her b eccentricity and inclination: Xiao
''et al.'' (2025)<ref name=Xiao2025/><br>14 Her c's other properties: Bardalez Gagliuffi ''et al.'' (2025)<ref name="Bardalez-Gagliuffi2025"/>}}
| period_unit = year
| period_unit = year
}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = [[14 Herculis b|b]]
| exoplanet = [[14 Herculis b|b]]
| mass = {{val|8.5|1.0|0.8}}
| mass = {{val|8.9|1.1|1.5}}
| period = {{val|4.8393|0.0006}}
| period = {{val|4.8285|0.0022|0.0023}}
| semimajor = {{val|2.845|0.038|0.039}}
| semimajor = {{val|2.843|0.040}}
| eccentricity = {{val|0.372|0.001}}
| eccentricity = {{val|0.371|0.003}}
| inclination = {{val|35.7|3.2}}
| inclination = {{val|147.3|2.2|2.7}}
}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = [[14 Herculis c|c]]
| exoplanet = [[14 Herculis c|c]]
| mass = {{val|7.1|1.0|0.6}}
| mass = {{val|7.9|1.6|1.2}}
| period = {{val|142.8|2.8}}
| period = {{val|143|3}}
| semimajor = {{val|27.4|16|7.9}}
| semimajor ={{val|20.0|12.0|4.9|ul=AU}}
| eccentricity = {{val|0.65|0.06}}
| eccentricity = {{val|0.52|0.16|0.12}}
| inclination = {{val|82|14}}
| inclination = {{val|111.9|5.4|4.5|u=deg}}
| radius = {{val|1.03|0.01}}
}}
}}
{{Orbitbox end}}
{{Orbitbox end}}
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* [[47 Ursae Majoris]]
* [[47 Ursae Majoris]]
* [[List of stars in Hercules]]
* [[List of stars in Hercules]]
* [[Lists of exoplanets]]
 
==Notes==
{{Notelist}}


== References ==
== References ==
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<ref name="GaiaDR3">{{Cite Gaia DR3|1385293808145621504}}</ref>
<ref name="GaiaDR3">{{Cite Gaia DR3|1385293808145621504}}</ref>
<ref name="Bardalez-Gagliuffi2025">{{cite journal |last1=Bardalez Gagliuffi |first1=Daniella |last2=Balmer |first2=William O. |display-authors=etal |date=June 2025 |title=JWST Coronagraphic Images of 14 Her c: a Cold Giant Planet in a Dynamically Hot, Multi-planet System |journal=[[The Astrophysical Journal Letters]] |volume= |issue= |pages= |doi= |arxiv=2506.09201}}</ref>


<ref name="von Braun2014">{{cite journal | title=Stellar diameters and temperatures - V. 11 newly characterized exoplanet host stars | last1=von Braun | first1=Kaspar | last2=Boyajian | first2=Tabetha S. | last3=van Belle | first3=Gerard T. | last4=Kane | first4=Stephen R. | last5=Jones | first5=Jeremy | last6=Farrington | first6=Chris | last7=Schaefer | first7=Gail | last8=Vargas | first8=Norm | last9=Scott | first9=Nic | last10=ten Brummelaar | first10=Theo A. | last11=Kephart | first11=Miranda | last12=Gies | first12=Douglas R. | last13=Ciardi | first13=David R. | last14=López-Morales | first14=Mercedes | last15=Mazingue | first15=Cassidy | last16=McAlister | first16=Harold A. | last17=Ridgway | first17=Stephen | last18=Goldfinger | first18=P. J. | last19=Turner | first19=Nils H. | last20=Sturmann | first20=Laszlo | display-authors=1 | journal=Monthly Notices of the Royal Astronomical Society | volume=438 | issue=3 | pages=2413–2425 | year=2014 | arxiv=1312.1792 | bibcode=2014MNRAS.438.2413V | doi=10.1093/mnras/stt2360 | doi-access=free }}</ref>
<ref name="von Braun2014">{{cite journal | title=Stellar diameters and temperatures - V. 11 newly characterized exoplanet host stars | last1=von Braun | first1=Kaspar | last2=Boyajian | first2=Tabetha S. | last3=van Belle | first3=Gerard T. | last4=Kane | first4=Stephen R. | last5=Jones | first5=Jeremy | last6=Farrington | first6=Chris | last7=Schaefer | first7=Gail | last8=Vargas | first8=Norm | last9=Scott | first9=Nic | last10=ten Brummelaar | first10=Theo A. | last11=Kephart | first11=Miranda | last12=Gies | first12=Douglas R. | last13=Ciardi | first13=David R. | last14=López-Morales | first14=Mercedes | last15=Mazingue | first15=Cassidy | last16=McAlister | first16=Harold A. | last17=Ridgway | first17=Stephen | last18=Goldfinger | first18=P. J. | last19=Turner | first19=Nils H. | last20=Sturmann | first20=Laszlo | display-authors=1 | journal=Monthly Notices of the Royal Astronomical Society | volume=438 | issue=3 | pages=2413–2425 | year=2014 | arxiv=1312.1792 | bibcode=2014MNRAS.438.2413V | doi=10.1093/mnras/stt2360 | doi-access=free }}</ref>
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  | arxiv=1411.4302 | s2cid=54555839 }}</ref>
  | arxiv=1411.4302 | s2cid=54555839 }}</ref>


<ref name=Anderson2012>{{citation
<ref name=Anderson2012>{{cite journal
  | title=XHIP: An extended hipparcos compilation
  | title=XHIP: An extended hipparcos compilation
  | last1=Anderson | first1=E. | last2=Francis | first2=Ch.
  | last1=Anderson | first1=E. | last2=Francis | first2=Ch.
Line 107: Line 117:
  | volume=38 | issue=5 | pages=331 | year=2012
  | volume=38 | issue=5 | pages=331 | year=2012
  | bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015
  | bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015
  | arxiv=1108.4971 | s2cid=119257644 | postscript=. }}</ref>
  | arxiv=1108.4971 | s2cid=119257644 }}</ref>
 
<ref name=Xiao2025>{{cite arXiv|eprint=2506.13580 |last1=Xiao |first1=Guang-Yao |last2=Feng |first2=Fabo |title=Updated Mutual Inclination Measurement for 14 Her b and C |date=2025 |class=astro-ph.EP }}</ref>


<ref name="Gagliuffi2021">{{cite journal | last1=Bardalez Gagliuffi | first1=Daniella C. |author-link1=Daniella Bardalez Gagliuffi | last2=Faherty | first2=Jacqueline K. | last3=Li | first3=Yiting | last4=Brandt | first4=Timothy D. | last5=Williams | first5=Lauryn | last6=Brandt | first6=G. Mirek | last7=Gelino | first7=Christopher R. | display-authors=1 | title=14 Her: A Likely Case of Planet–Planet Scattering | journal=The Astrophysical Journal Letters | date=1 December 2021 | volume=922 | issue=2 | at=L43 | arxiv=2111.06004 | bibcode=2021ApJ...922L..43B | bibcode-access=free | doi=10.3847/2041-8213/ac382c | doi-access=free }}</ref>
<ref name="Gagliuffi2021">{{cite journal | last1=Bardalez Gagliuffi | first1=Daniella C. |author-link1=Daniella Bardalez Gagliuffi | last2=Faherty | first2=Jacqueline K. | last3=Li | first3=Yiting | last4=Brandt | first4=Timothy D. | last5=Williams | first5=Lauryn | last6=Brandt | first6=G. Mirek | last7=Gelino | first7=Christopher R. | display-authors=1 | title=14 Her: A Likely Case of Planet–Planet Scattering | journal=The Astrophysical Journal Letters | date=1 December 2021 | volume=922 | issue=2 | at=L43 | arxiv=2111.06004 | bibcode=2021ApJ...922L..43B | bibcode-access=free | doi=10.3847/2041-8213/ac382c | doi-access=free }}</ref>


<ref name=perkins1989>{{citation
<ref name=perkins1989>{{cite journal
  | title=The Perkins catalog of revised MK types for the cooler stars
  | title=The Perkins catalog of revised MK types for the cooler stars
  | last1=Keenan | first1=Philip C. | last2=McNeil | first2=Raymond C.
  | last1=Keenan | first1=Philip C. | last2=McNeil | first2=Raymond C.
  | journal=Astrophysical Journal Supplement Series
  | journal=Astrophysical Journal Supplement Series
  | volume=71 | pages=245 | year=1989 | postscript=.
  | volume=71 | pages=245 | year=1989
  | bibcode=1989ApJS...71..245K | doi=10.1086/191373 }}</ref>
  | bibcode=1989ApJS...71..245K | doi=10.1086/191373 }}</ref>


<ref name="press release">{{cite press release | title=14 Herculis: A NEW EXTRASOLAR PLANET DISCOVERED AT THE HAUTE PROVENCE OBSERVATORY | author=Elisabeth Teichmann | date=1998-07-06 | publisher=L'Observatoire de Haute-Provence | location=France | url=http://www.obs-hp.fr/www/nouvelles/14her.html | access-date=2022-01-01 }}</ref>
<ref name="press release">{{cite press release | title=14 Herculis: A NEW EXTRASOLAR PLANET DISCOVERED AT THE HAUTE PROVENCE OBSERVATORY | author=Elisabeth Teichmann | date=1998-07-06 | publisher=L'Observatoire de Haute-Provence | location=France | url=http://www.obs-hp.fr/www/nouvelles/14her.html | access-date=2022-01-01 }}</ref>
<ref name=Feng2024>{{Cite journal |last1=Feng |first1=Fabo |last2=Xiao |first2=Guang-Yao |last3=Jones |first3=Hugh R A |last4=Jenkins |first4=James S |last5=Pena |first5=Pablo |last6=Sun |first6=Qinghui |date=2024-12-19 |title=Lessons learned from the detection of wide companions by radial velocity and astrometry |journal=Monthly Notices of the Royal Astronomical Society |volume=539 |issue=4 |pages=3180–3200 |doi=10.1093/mnras/staf689 |doi-access=free |arxiv=2412.14542 |issn=0035-8711}}</ref>


<ref name="wittenmyer">{{cite journal | display-authors=1 |first1=Robert A. | last1=Wittenmyer | last2=Endl | first2=Michael | last3=Cochran | first3=William D. | date=January 2007 | title=Long-Period Objects in the Extrasolar Planetary Systems 47 Ursae Majoris and 14 Herculis | journal=The Astrophysical Journal | volume=654 | issue=1 | pages=625–632 | arxiv=astro-ph/0609117 | bibcode=2007ApJ...654..625W | bibcode-access=free | doi=10.1086/509110 | doi-access=free | s2cid=14707902 }}</ref>
<ref name="wittenmyer">{{cite journal | display-authors=1 |first1=Robert A. | last1=Wittenmyer | last2=Endl | first2=Michael | last3=Cochran | first3=William D. | date=January 2007 | title=Long-Period Objects in the Extrasolar Planetary Systems 47 Ursae Majoris and 14 Herculis | journal=The Astrophysical Journal | volume=654 | issue=1 | pages=625–632 | arxiv=astro-ph/0609117 | bibcode=2007ApJ...654..625W | bibcode-access=free | doi=10.1086/509110 | doi-access=free | s2cid=14707902 }}</ref>

Latest revision as of 14:30, 28 June 2025

Template:Short description

14 Herculis
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]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)+5.39[2]
Details[4]
MassTemplate:Val Template:Solar mass
RadiusTemplate:Val Template:Solar radius
LuminosityTemplate:Val[5] Template:Solar luminosity
Surface gravity (log g)4.46 cgs
TemperatureTemplate:Val K
Metallicity [Fe/H]Template:Val dex
Rotation29.5 d
Rotational velocity (v sin i)1.65 km/s
AgeTemplate:Val[6] Gyr
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Template:Odlist[7]
Database references
SIMBADdata
Exoplanet Archivedata

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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

Template:Notelist

References

Template:Reflist

External links

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Template:14 Herculis Template:Stars of Hercules Template:Sky

  1. ↑ a b c d Cite error: Invalid <ref> tag; no text was provided for refs named GaiaDR3
  2. ↑ a b c d Cite error: Invalid <ref> tag; no text was provided for refs named Anderson2012
  3. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named perkins1989
  4. ↑ a b c d Cite error: Invalid <ref> tag; no text was provided for refs named Gagliuffi2021
  5. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named von Braun2014
  6. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Bonfanti2015
  7. ↑ Template:Cite simbad
  8. ↑ S. Feltzing and G. Gonzalez, "The nature of super-metal-rich stars* Detailed abundance analysis of 8 super-metal-rich star candidates", 2001
  9. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named press release
  10. ↑ Script error: No such module "citation/CS1".
  11. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Butler2003
  12. ↑ a b Cite error: Invalid <ref> tag; no text was provided for refs named wittenmyer
  13. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Gozdziewski2006
  14. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Rosenthal2021
  15. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named Feng2022
  16. ↑ a b Cite error: Invalid <ref> tag; no text was provided for refs named Benedict2023
  17. ↑ a b c Cite error: Invalid <ref> tag; no text was provided for refs named Bardalez-Gagliuffi2025
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