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GJ 3379

Coordinates:Sky map06h00m3.495s,+02° 42′ 23.67″
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GJ 3379
Observation data
EpochJ2000.0EquinoxJ2000.0
Constellation Orion
Right ascension 06h00m03.50386s[1]
Declination +02° 42′ 23.5968″[1]
Apparent magnitude(V) +11.307[2]
Characteristics
Spectral type M3.5Ve[3]or dM4.0[4]
B−Vcolor index 1.667[2]
Astrometry
Radial velocity(Rv)+30.228±0.0038[5]km/s
Proper motion(μ)RA:+309.487[1]mas/yr
Dec.:−40.640[1]mas/yr
Parallax(π)192.0135 ± 0.0310mas[6]
Distance16.986 ± 0.003ly
(5.2080 ± 0.0008pc)
Absolute magnitude(MV)+12.71[3]
Details[4]
Mass0.2312±0.0058M☉
Radius0.2457±0.0078R☉
Luminosity0.006329±0.000088L☉
Luminosity (bolometric)0.0086[7]L☉
Surface gravity(logg)5.10±0.07cgs
Temperature3,284±51K
Metallicity[Fe/H]−0.12±0.16dex
Rotation1.809 d[8]
Rotational velocity(vsini)5.8±0.3 km/s[3]km/s
Other designations
GJ3379,WDSJ06001+0242A,G99-49,G106-17,LTT17897,NLTT15908,PLX1383.02,TYC134-605-1,2MASSJ06000351+0242236[9]
Database references
SIMBADdata
GJ 3379 is located in the constellation Orion
GJ 3379 is located in the constellation Orion
GJ 3379
Location of GJ 3379 in the constellationOrion

GJ 3379(Giclas 99-49) is the neareststarin theOrionconstellation, located at a distance of 17light yearsfrom theSunbased onparallax.It is a single star[3]with anapparent visual magnitudeof +11.31[2]and anabsolute magnitudeof +12.71,[3]therefore, the star is not visible with the naked eye. It is positioned in the upper left part of the Orion constellation, to the SSE ofBetelgeuse.This star is drifting further away with aradial velocityof +30.0 kilometers per second.[5]In the past, this star had a relatively close encounter with theSolar System.Some161,000±6,000 yearsago, it achieved a minimum distance of 4.08 ± 0.20 ly (1.25 ± 0.06 pc).[10]

Physical characteristics

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This star is a smallred dwarfwith astellar classificationof M3.5V[3]– anM-type main-sequence star.It is much smaller, cooler, and less massive than the Sun, radiating only 0.6% of the Sun's luminosity.[4]This is a veryactive[11]star that varies in brightness with an amplitude of0.0074±0.0029magnitude, modulated by a rapidrotation periodof 1.8 days.[8]Themagnetic fieldstrength has been measured as2.3 kG.It is a source ofX-ray emissionwith a luminosity of9.5×1027erg s−1.[12]

According to theSIMBADdatabase, the star is classified as aneruptive variable.[9]

References

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  1. ^abcdBrown, A. G. A.;et al. (Gaia collaboration) (August 2018)."GaiaData Release 2: Summary of the contents and survey properties ".Astronomy & Astrophysics.616.A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051.Gaia DR2 record for this sourceatVizieR.
  2. ^abcZacharias, N.; et al. (2012). "The fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)".VizieR On-line Data Catalog.1322.Bibcode:2012yCat.1322....0Z.
  3. ^abcdefDavison, Cassy L.; et al. (March 2015). "A 3D Search for Companions to 12 Nearby M-Dwarfs".The Astronomical Journal.149(3): 106.arXiv:1501.05012.Bibcode:2015AJ....149..106D.doi:10.1088/0004-6256/149/3/106.S2CID9719725.
  4. ^abcSchweitzer, A.; et al. (May 2019). "The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars".Astronomy & Astrophysics.625:16.arXiv:1904.03231.Bibcode:2019A&A...625A..68S.doi:10.1051/0004-6361/201834965.S2CID102351979.A68.
  5. ^abSoubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars".Astronomy and Astrophysics.616:A7.arXiv:1804.09370.Bibcode:2018A&A...616A...7S.doi:10.1051/0004-6361/201832795.S2CID52952408.
  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. ^Khata, Dhrimadri; et al. (April 2020). "Understanding the physical properties of young M dwarfs: NIR spectroscopic studies".Monthly Notices of the Royal Astronomical Society.493(3): 4533–4550.arXiv:2002.05762.Bibcode:2020MNRAS.493.4533K.doi:10.1093/mnras/staa427.
  8. ^abNewton, Elisabeth R.; et al. (April 2016)."The Rotation and Galactic Kinematics of Mid M Dwarfs in the Solar Neighborhood".The Astrophysical Journal.821(2): 21.arXiv:1511.00957.Bibcode:2016ApJ...821...93N.doi:10.3847/0004-637X/821/2/93.S2CID89615849.93.
  9. ^ab"G 99-49".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved18 August2017.
  10. ^Bobylev, V. V. (2017). "Search for close stellar encounters with the solar system from data on nearby dwarfs".Astronomy Reports.61(10): 883–890.arXiv:1708.03300.Bibcode:2017ARep...61..883B.doi:10.1134/S106377291710002X.ISSN1063-7729.S2CID119424830.
  11. ^Zechmeister, M.; et al. (January 2018). "Spectrum radial velocity analyser (SERVAL). High-precision radial velocities and two alternative spectral indicators".Astronomy & Astrophysics.609:13.arXiv:1710.10114.Bibcode:2018A&A...609A..12Z.doi:10.1051/0004-6361/201731483.S2CID59449762.A12.
  12. ^Feiden, Gregory A.; Chaboyer, Brian (December 2013). "Magnetic Inhibition of Convection and the Fundamental Properties of Low-mass Stars. I. Stars with a Radiative Core".The Astrophysical Journal.779(2): 25.arXiv:1309.0033.Bibcode:2013ApJ...779..183F.doi:10.1088/0004-637X/779/2/183.S2CID118558471.183.
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