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Gliese 251

Coordinates:Sky map06h54m48.96009s,+33° 16′ 05.4393″
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Gliese 251
Observation data
EpochJ2000EquinoxJ2000
Constellation Gemini
Right ascension 06h54m48.96009s[1]
Declination +33° 16′ 05.4393″[1]
Apparent magnitude(V) +10.11[2]
Characteristics
Spectral type M3.0Ve[3]
U−Bcolor index +1.20[4]
B−Vcolor index +1.60[4]
Astrometry
Radial velocity(Rv)22.91[5]km/s
Proper motion(μ)RA:-723.99[1]mas/yr
Dec.:-398.40[1]mas/yr
Parallax(π)179.0629 ± 0.0280mas[6]
Distance18.215 ± 0.003ly
(5.5846 ± 0.0009pc)
Absolute magnitude(MV)11.23[7]
Details
Mass0.360±0.015[8]M☉
Radius0.364±0.011[8]R☉
Surface gravity(logg)4.96±0.07[8]cgs
Temperature3451±51[8]K
Metallicity[Fe/H]-0.03±0.16[8]dex
Rotational velocity(vsini)≤2[8]km/s
Other designations
Gliese251,HD265866,HIP33226,LHS1879,LTT11941,Ross578,Wolf294,2MASSJ06544902+3316058[9]
Database references
SIMBADdata
ARICNSdata
Gliese 251 is located in the constellation Gemini
Gliese 251 is located in the constellation Gemini
Gliese 251
Location of Gliese 251 in the constellationGemini

Gliese 251,also known asHIP 33226orHD 265866,is astarlocated about 18light yearsaway from theSolar System.Located in theconstellationofGemini,it is the nearest star in this constellation.[10]It is located near the boundary withAuriga,49 arcminutes away from the bright starTheta Geminorum;due to itsapparent magnitudeof +9.89 it cannot be observed with the naked eye.[2]The closest star to Gliese 251 isQY Aurigae,which is located 3.5light yearsaway.[11]

Gliese 251 is ared dwarfwith aspectral typeof M3V[3]with an effective temperature of about 3300K.[3]Its mass has been measured to be around 0.36solar masses[8]and its radius is about 36%solar radii.[8]Itsmetallicityis likely slightly less than that of the Sun.[8]Observations at infrared wavelengths rule out the presence of a circumstellar disk around it.[12]

Planetary system

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In 2019, two candidate planets were detected by theradial velocity methodto orbit Gliese 251 at orbits of 1.74 and 607 days.[13]However, a new study in 2020 usingCARMENESdata refuted both candidates, as they found that both signals were caused by stellar activity. Based on the CARMENES data, the team announced that Gliese 251 is orbited by one singlesuper-Earth(Gliese 251 b) at an orbit of 14.238 days.[8]

The Gliese 251 planetary system[8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥4.0±0.4M🜨 0.0818+0.0011
−0.0012 		14.238±0.002 0.10+0.09
−0.07 		— —

See also

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References

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  1. ^abcdvan Leeuwen, F.; et al. (2007)."Validation of the new Hipparcos reduction".Astronomy and Astrophysics.474(2): 653–664.arXiv:0708.1752.Bibcode:2007A&A...474..653V.doi:10.1051/0004-6361:20078357.S2CID18759600.Archivedfrom the original on 2019-12-07.Retrieved2017-02-09.
  2. ^abHøg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars".Astronomy and Astrophysics.355:L27–L30.Bibcode:2000A&A...355L..27H.
  3. ^abcLépine, Sébastien (2013). "A Spectroscopic Catalog of the Brightest (J < 9) M Dwarfs in the Northern Sky".The Astronomical Journal.145(4): 102.arXiv:1206.5991.Bibcode:2013AJ....145..102L.doi:10.1088/0004-6256/145/4/102.S2CID117144290.
  4. ^abMermilliod, J.-C. (1986)."Compilation of Eggen's UBV data, transformed to UBV (unpublished)".Catalogue of Eggen's UBV Data.Bibcode:1986EgUBV........0M.Archivedfrom the original on 2019-12-08.Retrieved2017-02-09.
  5. ^Nidever, David L.; et al. (2013). "Radial Velocities for 889 Late-Type Stars".The Astrophysical Journal Supplement Series.141(2): 503–522.arXiv:astro-ph/0112477.Bibcode:2002ApJS..141..503N.doi:10.1086/340570.S2CID51814894.
  6. ^Brown, A. G. A.;et al. (Gaia collaboration) (2021)."GaiaEarly Data Release 3: Summary of the contents and survey properties ".Astronomy & Astrophysics.649:A1.arXiv:2012.01533.Bibcode:2021A&A...649A...1G.doi:10.1051/0004-6361/202039657.S2CID227254300.(Erratum:doi:10.1051/0004-6361/202039657e).Gaia EDR3 record for this sourceatVizieR.
  7. ^"ARICNS 4C00526".ARICNS.Archivedfrom the original on 31 August 2021.Retrieved8 February2017.
  8. ^abcdefghijkStock, S.; et al. (2020), "The CARMENES search for exoplanets around M dwarfs Three temperate-to-warm super-Earths",Astronomy & Astrophysics,A112:643,arXiv:2010.00474,Bibcode:2020A&A...643A.112S,doi:10.1051/0004-6361/202038820,S2CID222090233
  9. ^"GJ 251".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved8 February2017.
  10. ^"Closest Stars".Archivedfrom the original on 11 April 2023.Retrieved8 February2017.
  11. ^"Stars within 15 light-years of Wolf 294".The Internet Stellar Database.Retrieved7 February2017.
  12. ^Beichman, C. A.; et al. (2006). "New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets".The Astrophysical Journal.652(2): 1674–1693.arXiv:astro-ph/0611682.Bibcode:2006ApJ...652.1674B.doi:10.1086/508449.S2CID14207148.
  13. ^Barnes, J. R.; et al. (2019-06-11). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood".arXiv:1906.04644[astro-ph.EP].

Notes

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