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Coordinates: Sky map 08h 44m 25.7033s, +01° 51′ 36.1066″
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{{Short description|Star in the constellation Hydra}}
{{Starbox begin
{{Starbox begin}}
|name=BD+02 2056
⚫
}}
{{Starbox observe
{{Starbox observe
| epoch = J2000
| epoch = J2000
| constell = [[Hydra (constellation)|Hydra]]
| constell = [[Hydra (constellation)|Hydra]]
| ra = {{RA|08|44|25.7033}}<ref name=SIMBAD/>
| ra = {{RA|08|44|25.70315}}<ref name=GaiaDR3/>
| dec = {{DEC|+01|51|36.1066}}<ref name=SIMBAD/>
| dec = {{DEC|+01|51|36.1055}}<ref name=GaiaDR3/>
| appmag_v = 10.83
| appmag_v = 10.83
}}
}}
{{Starbox character
{{Starbox character
| type = [[main-sequence star]]
| type = [[main-sequence star]]
| class = G9V<ref name=Anderson2014/>
| class = G9V<ref name=Anderson2014/>
}}
}}
{{Starbox astrometry
{{Starbox astrometry
| radial_v = −5.1{{±|0.6}}<ref name=EDR3>{{cite Gaia EDR3|3078836109158636928}}</ref>
| radial_v = {{val|−11.63|0.21}}<ref name=GaiaDR3/>
| prop_mo_ra = −23.344<ref name=EDR3/>
| prop_mo_ra = −23.344
| prop_mo_dec = −31.570<ref name=EDR3/>
| prop_mo_dec = −31.570
| pm_footnote = <ref name=GaiaDR3/>
| parallax = 9.9636
| parallax = 9.9636
| p_error = 0.0149
| p_error = 0.0149
| parallax_footnote = <ref name=EDR3/>
| parallax_footnote = <ref name=GaiaDR3/>
}}
}}
{{Starbox detail
{{Starbox detail
Line 25: Line 25:
| mass = 0.842{{±|0.037|0.036}}
| mass = 0.842{{±|0.037|0.036}}
| radius = 0.748{{±|0.015}}
| radius = 0.748{{±|0.015}}
| temperature = 5350{{±|31}}<ref name=Teske2019/>
⚫
| temperature = 5350{{±|31}}<ref name=Teske2019>{{citation |arxiv=1912.00255 |doi=10.3847/1538-3881/ab4f79 |title=Do Metal-rich Stars Make Metal-rich Planets? New Insights on Giant Planet Formation from Host Star Abundances |year=2019 |last1=Teske |first1=Johanna K. |last2=Thorngren |first2=Daniel |last3=Fortney |first3=Jonathan J. |last4=Hinkel |first4=Natalie |last5=Brewer |first5=John M. |journal=The Astronomical Journal |volume=158 |issue=6 |page=239 |bibcode=2019AJ....158..239T |s2cid=208527082 }}</ref>
| luminosity =
| luminosity =
| gravity = 4.63{{±|0.06}}<ref name=Teske2019/>
| gravity = 4.63{{±|0.06}}<ref name=Teske2019/>
| metal_fe = 0.05{{±|0.02}}<ref name=Teske2019/>
| metal_fe = 0.05{{±|0.02}}<ref name=Teske2019/>
Line 34: Line 34:
}}
}}
{{Starbox catalog
{{Starbox catalog
| names = {{odlist|2MASS = J08442570+0151361|Gaia DR2=3078836109158636928|WASP=84|TYC=211-706-1|GSC=00211-00706}}<ref name=SIMBAD>{{cite simbad|title=BD+02 2056|access-date=2021-01-25}}</ref>
| names = {{odlist|2MASS = J08442570+0151361 | BD = +02 2056 |Gaia DR2=3078836109158636928|WASP=84|TYC=211-706-1|GSC=00211-00706}}<ref name=SIMBAD/>
}}
}}
{{Starbox reference
{{Starbox reference
| Simbad = BD+02 2056
| Simbad = WASP-84
}}
}}
{{Starbox end}}
{{Starbox end}}


'''BD+02 2056''', also known as '''WASP-84''' is a [[G-type main-sequence star]]. Its surface temperature is 5350{{±|31}} [[Kelvin|K]], and is slightly enriched in heavy elements compared to the [[Sun]], with a [[metallicity]] Fe/H index of 0.05{{±|0.02}}. It is rich in carbon and depleted of oxygen.<ref name=Teske2019/> BD+02 2056's age is probably older than the [[Sun]] at 8.5{{±|4.1|5.5}} billion years.<ref name=Bonomo2017/> The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.<ref>{{citation |arxiv=1503.09111 |doi=10.1051/0004-6361/201525774 |title=Comparison of gyrochronological and isochronal age estimates for transiting exoplanet host stars |year=2015 |last1=Maxted |first1=P. F. L. |last2=Serenelli |first2=A. M. |last3=Southworth |first3=J. |journal=Astronomy & Astrophysics |volume=577 |pages=A90 |bibcode=2015A&A...577A..90M |s2cid=53324330 }}</ref>
'''WASP-84''', also known as '''BD+02 2056''', is a [[G-type main-sequence star]] {{convert|327|ly|pc|lk=on|abbr=off}} away in the constellation [[Hydra (constellation)|Hydra]]. Its surface temperature is 5350{{±|31}} [[Kelvin|K]] and is slightly enriched in heavy elements compared to the [[Sun]], with a [[metallicity]] Fe/H index of 0.05{{±|0.02}}. It is rich in carbon and depleted of oxygen.<ref name=Teske2019/> WASP-84's age is probably older than the [[Sun]] at 8.5{{±|4.1|5.5}} billion years.<ref name=Bonomo2017/> The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.<ref>{{citation |arxiv=1503.09111 |doi=10.1051/0004-6361/201525774 |title=Comparison of gyrochronological and isochronal age estimates for transiting exoplanet host stars |year=2015 |last1=Maxted |first1=P. F. L. |last2=Serenelli |first2=A. M. |last3=Southworth |first3=J. |journal=Astronomy & Astrophysics |volume=577 |pages=A90 |bibcode=2015A&A...577A..90M |s2cid=53324330 }}</ref>


A multiplicity survey did not detect any stellar companions to BD+02 2056 as at 2015.<ref>{{citation |arxiv=1506.05456 |doi=10.1051/0004-6361/201526525 |title=A Lucky Imaging search for stellar sources near 74 transit hosts |year=2015 |last1=Wöllert |first1=Maria |last2=Brandner |first2=Wolfgang |journal=Astronomy & Astrophysics |volume=579 |pages=A129 |bibcode=2015A&A...579A.129W |s2cid=118903879 }}</ref>
A multiplicity survey did not detect any stellar companions to WASP-84 as of 2015.<ref>{{citation |arxiv=1506.05456 |doi=10.1051/0004-6361/201526525 |title=A Lucky Imaging search for stellar sources near 74 transit hosts |year=2015 |last1=Wöllert |first1=Maria |last2=Brandner |first2=Wolfgang |journal=Astronomy & Astrophysics |volume=579 |pages=A129 |bibcode=2015A&A...579A.129W |s2cid=118903879 }}</ref>


==Planetary system==
==Planetary system==
In 2013, one [[exoplanet]], named [[WASP-84b]], was discovered on a tight, circular orbit.<ref name="Anderson2013"/> The planet is a [[hot Jupiter]] that cannot have formed in its current location and likely migrated from elsewhere. The planetary orbit is well aligned with the equatorial plane of the star, misalignment being equal to 0.3{{±|1.7}}°. Planetary equilibrium temperature is 832{{±|13}} [[Kelvin|K]].<ref name=Anderson2014/>
⚫
In 2013, one planet, named [[WASP-84b]], was discovered on a tight, circular orbit.<ref>{{citation |arxiv=1310.5654 |doi=10.1093/mnras/stu1737 |title=Three newly discovered sub-Jupiter-mass planets: WASP-69b and WASP-84b transit active K dwarfs and WASP-70Ab transits the evolved primary of a G4+K3 binary★† |year=2014 |last1=Anderson |first1=D. R. |last2=Collier Cameron |first2=A. |last3=Delrez |first3=L. |last4=Doyle |first4=A. P. |last5=Faedi |first5=F. |last6=Fumel |first6=A. |last7=Gillon |first7=M. |last8=Gómez Maqueo Chew |first8=Y. |last9=Hellier |first9=C. |last10=Jehin |first10=E. |last11=Lendl |first11=M. |last12=Maxted |first12=P. F. L. |last13=Pepe |first13=F. |last14=Pollacco |first14=D. |last15=Queloz |first15=D. |last16=Ségransan |first16=D. |last17=Skillen |first17=I. |last18=Smalley |first18=B. |last19=Smith |first19=A. M. S. |last20=Southworth |first20=J. |last21=Triaud |first21=A. H. M. J. |last22=Turner |first22=O. D. |last23=Udry |first23=S. |last24=West |first24=R. G. |journal=Monthly Notices of the Royal Astronomical Society |volume=445 |issue=2 |pages=1114–1129 |s2cid=54750890 }}</ref> The planet cannot have formed in its current location and likely migrated from elsewhere. The planetary orbit is well aligned with the equatorial plane of the star, misalignment being equal to 0.3{{±|1.7}}°. Planetary equilibrium temperature is 832{{±|13}} [[Kelvin|K]].<ref name=Anderson2014>{{citation |arxiv=1409.6335 |doi=10.1088/2041-8205/800/1/L9 |title=THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF a HOT JUPITER |year=2015 |last1=Anderson |first1=D. R. |last2=Triaud |first2=A. H. M. J. |last3=Turner |first3=O. D. |last4=Brown |first4=D. J. A. |last5=Clark |first5=B. J. M. |last6=Smalley |first6=B. |last7=Cameron |first7=A. Collier |last8=Doyle |first8=A. P. |last9=Gillon |first9=M. |last10=Hellier |first10=C. |last11=Lovis |first11=C. |last12=Maxted |first12=P. F. L. |last13=Pollacco |first13=D. |last14=Queloz |first14=D. |last15=Smith |first15=A. M. S. |journal=The Astrophysical Journal |volume=800 |issue=1 |pages=L9 |bibcode=2015ApJ...800L...9A |s2cid=13606807 }}</ref>

In 2023, a second planet was discovered around WASP-84. This appears to be a dense [[rocky planet]] despite its high mass, comparable to [[Uranus]].<ref name="Maciejewski2023"/>

{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
| name = WASP-84
| name = WASP-84
| table_ref = <ref name="Maciejewski2023"/>
⚫
| table_ref =<ref name=Bonomo2017>{{citation |arxiv=1704.00373|title=The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets|year=2017|doi=10.1051/0004-6361/201629882|last1=Bonomo|first1=A. S.|last2=Desidera|first2=S.|last3=Benatti|first3=S.|last4=Borsa|first4=F.|last5=Crespi|first5=S.|last6=Damasso|first6=M.|last7=Lanza|first7=A. F.|last8=Sozzetti|first8=A.|last9=Lodato|first9=G.|last10=Marzari|first10=F.|last11=Boccato|first11=C.|last12=Claudi|first12=R. U.|last13=Cosentino|first13=R.|last14=Covino|first14=E.|last15=Gratton|first15=R.|last16=Maggio|first16=A.|last17=Micela|first17=G.|last18=Molinari|first18=E.|last19=Pagano|first19=I.|last20=Piotto|first20=G.|last21=Poretti|first21=E.|last22=Smareglia|first22=R.|last23=Affer|first23=L.|last24=Biazzo|first24=K.|last25=Bignamini|first25=A.|last26=Esposito|first26=M.|last27=Giacobbe|first27=P.|last28=Hébrard|first28=G.|last29=Malavolta|first29=L.|last30=Maldonado|first30=J.|journal=Astronomy & Astrophysics|volume=A107|page=602|bibcode=2017A&A...602A.107B|s2cid=118923163|display-authors=29}}</ref>
}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = [[WASP-84b|b]]
| exoplanet = c
| mass = 0.694{{±|0.049|0.047}}
| mass_earth = {{val|15.2|4.5|4.2}}
| radius = 0.942{{±|0.022}}
| radius_earth = {{val|1.95|0.12}}
| semimajor = 0.0771{{±|0.0011}}
| semimajor = {{val|0.02359|0.00100}}
| period = 8.5234865{{±|0.000007}}
| period = {{val|1.4468849|0.0000022|0.0000016}}
| eccentricity = <0.077
| eccentricity =
| inclination = 88.368{{±|0.050}}
| inclination = {{val|83.20|0.51|0.49}}
⚫
}}
{{OrbitboxPlanet
| exoplanet = b
| mass = {{val|0.692|0.058}}
| radius = {{val|0.956|0.024}}
| semimajor = {{val|0.0778|0.0021}}
| period = {{val|8.52349648|(60)}}
| eccentricity = <0.077<ref name=Bonomo2017/>
| inclination = {{val|88.292|0.045|0.042}}
}}
}}
{{Orbitbox end}}
{{Orbitbox end}}


==References==
==References==
{{Reflist}}
{{Reflist|refs=

<ref name=SIMBAD>{{cite simbad|title=BD+02 2056|access-date=2021-01-25}}</ref>

<ref name=GaiaDR3>{{cite Gaia DR3|3078836109158636928}}</ref>

⚫
<ref name="Anderson2013">{{citation |arxiv=1310.5654 |doi=10.1093/mnras/stu1737 |title=Three newly discovered sub-Jupiter-mass planets: WASP-69b and WASP-84b transit active K dwarfs and WASP-70Ab transits the evolved primary of a G4+K3 binary |year=2014 |last1=Anderson |first1=D. R. |last2=Collier Cameron |first2=A. |last3=Delrez |first3=L. |last4=Doyle |first4=A. P. |last5=Faedi |first5=F. |last6=Fumel |first6=A. |last7=Gillon |first7=M. |last8=Gómez Maqueo Chew |first8=Y. |last9=Hellier |first9=C. |last10=Jehin |first10=E. |last11=Lendl |first11=M. |last12=Maxted |first12=P. F. L. |last13=Pepe |first13=F. |last14=Pollacco |first14=D. |last15=Queloz |first15=D. |last16=Ségransan |first16=D. |last17=Skillen |first17=I. |last18=Smalley |first18=B. |last19=Smith |first19=A. M. S. |last20=Southworth |first20=J. |last21=Triaud |first21=A. H. M. J. |last22=Turner |first22=O. D. |last23=Udry |first23=S. |last24=West |first24=R. G. |journal=Monthly Notices of the Royal Astronomical Society |volume=445 |issue=2 |pages=1114–1129 |doi-access=free |s2cid=54750890 |bibcode=2014MNRAS.445.1114A}}</ref>

<ref name=Anderson2014>{{citation |arxiv=1409.6335 |doi=10.1088/2041-8205/800/1/L9 |title=THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF a HOT JUPITER |year=2015 |last1=Anderson |first1=D. R. |last2=Triaud |first2=A. H. M. J. |last3=Turner |first3=O. D. |last4=Brown |first4=D. J. A. |last5=Clark |first5=B. J. M. |last6=Smalley |first6=B. |last7=Cameron |first7=A. Collier |last8=Doyle |first8=A. P. |last9=Gillon |first9=M. |last10=Hellier |first10=C. |last11=Lovis |first11=C. |last12=Maxted |first12=P. F. L. |last13=Pollacco |first13=D. |last14=Queloz |first14=D. |last15=Smith |first15=A. M. S. |journal=The Astrophysical Journal |volume=800 |issue=1 |pages=L9 |bibcode=2015ApJ...800L...9A |s2cid=13606807 }}</ref>

⚫
<ref name=Bonomo2017>{{citation |arxiv=1704.00373|title=The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets|year=2017|doi=10.1051/0004-6361/201629882|last1=Bonomo|first1=A. S.|last2=Desidera|first2=S.|last3=Benatti|first3=S.|last4=Borsa|first4=F.|last5=Crespi|first5=S.|last6=Damasso|first6=M.|last7=Lanza|first7=A. F.|last8=Sozzetti|first8=A.|last9=Lodato|first9=G.|last10=Marzari|first10=F.|last11=Boccato|first11=C.|last12=Claudi|first12=R. U.|last13=Cosentino|first13=R.|last14=Covino|first14=E.|last15=Gratton|first15=R.|last16=Maggio|first16=A.|last17=Micela|first17=G.|last18=Molinari|first18=E.|last19=Pagano|first19=I.|last20=Piotto|first20=G.|last21=Poretti|first21=E.|last22=Smareglia|first22=R.|last23=Affer|first23=L.|last24=Biazzo|first24=K.|last25=Bignamini|first25=A.|last26=Esposito|first26=M.|last27=Giacobbe|first27=P.|last28=Hébrard|first28=G.|last29=Malavolta|first29=L.|last30=Maldonado|first30=J.|journal=Astronomy & Astrophysics|volume=A107|page=602|bibcode=2017A&A...602A.107B|s2cid=118923163|display-authors=29}}</ref>

⚫
<ref name=Teske2019>{{citation |arxiv=1912.00255 |doi=10.3847/1538-3881/ab4f79 |title=Do Metal-rich Stars Make Metal-rich Planets? New Insights on Giant Planet Formation from Host Star Abundances |year=2019 |last1=Teske |first1=Johanna K. |last2=Thorngren |first2=Daniel |last3=Fortney |first3=Jonathan J. |last4=Hinkel |first4=Natalie |last5=Brewer |first5=John M. |journal=The Astronomical Journal |volume=158 |issue=6 |page=239 |bibcode=2019AJ....158..239T |s2cid=208527082 |doi-access=free }}</ref>

<ref name="Maciejewski2023">{{cite journal |last1=Maciejewski |first1=G. |last2=Golonka |first2=J. |display-authors=etal |date=May 2023 |title=A hot super-Earth planet in the WASP-84 planetary system |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=525 |issue=1 |pages=L43–L49 |doi=10.1093/mnrasl/slad078 |doi-access=free |arxiv=2305.09177 |bibcode=2023MNRAS.525L..43M}}</ref>

}}


{{Sky|08|44|25.7033|+|01|51|36.1066}}
{{Sky|08|44|25.7033|+|01|51|36.1066}}
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[[Category:Planetary transit variables]]
[[Category:Planetary transit variables]]
[[Category:G-type main-sequence stars]]
[[Category:G-type main-sequence stars]]
[[Category:Planetary systems with one confirmed planet]]
[[Category:Planetary systems with two confirmed planets]]
[[Category:2MASS objects|J08442570+0151361]]
[[Category:2MASS objects|J08442570+0151361]]
[[Category:Durchmusterung objects|BD+02 2056]]
[[Category:Durchmusterung objects|BD+02 2056]]

Latest revision as of 21:28, 26 August 2024

WASP-84
Observation data
Epoch J2000      Equinox J2000
Constellation Hydra
Right ascension 08h 44m 25.70315s[1]
Declination +01° 51′ 36.1055″[1]
Apparent magnitude (V) 10.83
Characteristics
Evolutionary stage main-sequence star
Spectral type G9V[2]
Astrometry
Radial velocity (Rv)−11.63±0.21[1] km/s
Proper motion (μ) RA: −23.344 mas/yr[1]
Dec.: −31.570 mas/yr[1]
Parallax (π)9.9636 ± 0.0149 mas[1]
Distance327.3 ± 0.5 ly
(100.4 ± 0.2 pc)
Details[3]
Mass0.842+0.037
−0.036 M☉
Radius0.748±0.015 R☉
Surface gravity (log g)4.63±0.06[4] cgs
Temperature5350±31[4] K
Metallicity [Fe/H]0.05±0.02[4] dex
Rotation14.36±0.35 d
Rotational velocity (v sin i)4.10±0.30 km/s
Age8.5+4.1
−5.5 Gyr
Other designations
BD+02 2056, Gaia DR2 3078836109158636928, WASP-84, TYC 211-706-1, GSC 00211-00706, 2MASS J08442570+0151361[5]
Database references
SIMBADdata

WASP-84, also known as BD+02 2056, is a G-type main-sequence star 327 light-years (100 parsecs) away in the constellation Hydra. Its surface temperature is 5350±31 K and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen.[4] WASP-84's age is probably older than the Sun at 8.5+4.1
−5.5 billion years.[3] The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.[6]

A multiplicity survey did not detect any stellar companions to WASP-84 as of 2015.[7]

Planetary system

[edit]

In 2013, one exoplanet, named WASP-84b, was discovered on a tight, circular orbit.[8] The planet is a hot Jupiter that cannot have formed in its current location and likely migrated from elsewhere. The planetary orbit is well aligned with the equatorial plane of the star, misalignment being equal to 0.3±1.7°. Planetary equilibrium temperature is 832±13 K.[2]

In 2023, a second planet was discovered around WASP-84. This appears to be a dense rocky planet despite its high mass, comparable to Uranus.[9]

The WASP-84 planetary system[9]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
c 15.2+4.5
−4.2 M🜨 		0.02359±0.00100 1.4468849+0.0000022
−0.0000016 		— 83.20+0.51
−0.49° 		1.95±0.12 R🜨
b 0.692±0.058 MJ 0.0778±0.0021 8.52349648(60) <0.077[3] 88.292+0.045
−0.042° 		0.956±0.024 RJ

References

[edit]
  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b Anderson, D. R.; Triaud, A. H. M. J.; Turner, O. D.; Brown, D. J. A.; Clark, B. J. M.; Smalley, B.; Cameron, A. Collier; Doyle, A. P.; Gillon, M.; Hellier, C.; Lovis, C.; Maxted, P. F. L.; Pollacco, D.; Queloz, D.; Smith, A. M. S. (2015), "THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF a HOT JUPITER", The Astrophysical Journal, 800 (1): L9, arXiv:1409.6335, Bibcode:2015ApJ...800L...9A, doi:10.1088/2041-8205/800/1/L9, S2CID 13606807
  3. ^ a b c Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A.; Lodato, G.; Marzari, F.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; et al. (2017), "The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets", Astronomy & Astrophysics, A107: 602, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
  4. ^ a b c d Teske, Johanna K.; Thorngren, Daniel; Fortney, Jonathan J.; Hinkel, Natalie; Brewer, John M. (2019), "Do Metal-rich Stars Make Metal-rich Planets? New Insights on Giant Planet Formation from Host Star Abundances", The Astronomical Journal, 158 (6): 239, arXiv:1912.00255, Bibcode:2019AJ....158..239T, doi:10.3847/1538-3881/ab4f79, S2CID 208527082
  5. ^ "BD+02 2056". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-25.
  6. ^ Maxted, P. F. L.; Serenelli, A. M.; Southworth, J. (2015), "Comparison of gyrochronological and isochronal age estimates for transiting exoplanet host stars", Astronomy & Astrophysics, 577: A90, arXiv:1503.09111, Bibcode:2015A&A...577A..90M, doi:10.1051/0004-6361/201525774, S2CID 53324330
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