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Gliese 179

Coordinates:Sky map04h 52m 05.7273s, +06° 28′ 35.542″
From Wikipedia, the free encyclopedia
Star in the constellation Orion
Gliese 179
Observation data
Epoch J2000.0      Equinox J2000.0
ConstellationOrion
Right ascension04h 52m 05.73212s[1]
Declination+06° 28′ 35.5887″[1]
Apparent magnitude (V)11.94[2]
Characteristics
Spectral typeM2V[3] or M3.5[4]
Apparent magnitude (U)14.791[2]
Apparent magnitude (B)13.530[2]
Apparent magnitude (R)10.85[2]
Apparent magnitude (I)9.334[2]
Apparent magnitude (J)7.814±0.024[2]
Apparent magnitude (H)7.209±0.046[2]
Apparent magnitude (K)6.942±0.018[2]
U−Bcolor index1.26[2]
B−Vcolor index1.590±0.015[2]
V−Rcolor index1.09[2]
R−Icolor index1.52[2]
Astrometry
Radial velocity (Rv)–9.05±0.15[2] km/s
Proper motion (μ)RA: 153.615mas/yr[1]
Dec.: −306.046mas/yr[1]
Parallax (π)80.5623±0.0236 mas[1]
Distance40.48 ± 0.01 ly
(12.413 ± 0.004 pc)
Absolute magnitude (MV)11.50[2]
Details
Mass0.400±0.005 M☉[4]
0.357±0.03[5] M☉
Radius0.400±0.005 R☉[4]
0.318±0.024 R☉[6]
0.38±0.02[5] R☉
Luminosity0.0158±0.0003 L☉[4]
0.016±0.02[5] L☉
Surface gravity (log g)4.148[7] cgs
Temperature3,424±16[8] K
Metallicity[Fe/H]+0.36±0.04 dex[9]
+0.30±0.10 dex[5]
+0.12[10] dex
Age4.6+3.5
−2.4[10] Gyr
Other designations
GJ 179,HIP 22627,G 83-37, 84-15, 82-52,LTT 11525,NLTT 14088,Ross 401,Wolf 1539[11]
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata

Gliese 179 is a smallred dwarfstar with anexoplanetary companion in theequatorialconstellation ofOrion. It is much too faint to be visible to the naked eye with anapparent visual magnitude of 11.94.[2] The system is located at a distance of 40.5light-years (12.4parsecs) from theSun based onparallax measurements, but is drifting closer with aradial velocity of –9 km/s.[2] It is a highproper motion star, traversing thecelestial sphere at anangular rate of0.370″·yr−1.[12]

This is anM-type main-sequence star with astellar classification of M2V.[3] Based on the motion of this star through space, it is estimated to be roughly 4.6 billion years old.[10] It ischromospherically active[5] with aprojected rotational velocity of 4 km/s.[7] This star is smaller and less massive than the Sun, but has a highermetal content. It is radiating just 1.6% of the luminosity of the Sun from itsphotosphere at aneffective temperature of 3,424 K.[8]

In 2009, a Jovian-type planet was found in orbit around the star,[5] one of the few red dwarfs known to harbor a planet of this mass.[10] The radial velocity data suggested there may be an additional companion. At the orbital distance of this planet, it is not expected to be influenced by tidal interactions with the host star.[10] In 2023, the inclination and true mass of Gliese 179 b were determined viaastrometry.[13] A second candidate planet was reported in 2017[14] and was also reported in a 2019preprint. This is a potential super-Earth with a minimum mass equal to about five times the mass of the Earth.[15]

The Gliese 179 planetary system[13][15]
Companion
(in order from star)		MassSemimajor axis
(AU)		Orbital period
(days)		EccentricityInclinationRadius
c(unconfirmed)≥4.9±2.7M🜨0.032±0.0033.4798+0.0014
−0.0010		0.04+0.27
−0.04		——
b0.95+0.16
−0.11 MJ		2.424+0.071
−0.075		2303+34
−31		0.179+0.048
−0.044		61+16
−13 or119+13
−16°		—

See also

[edit]

References

[edit]
  1. ^abcdVallenari, 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 atVizieR.
  2. ^abcdefghijklmnopAnderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation".Astronomy Letters.38 (5): 331.arXiv:1108.4971.Bibcode:2012AstL...38..331A.doi:10.1134/S1063773712050015.S2CID 11925764.
  3. ^abStephenson, C. B. (July 1986)."Dwarf K and M stars of high proper motion found in a hemispheric survey".The Astronomical Journal.92:139–165.Bibcode:1986AJ.....92..139S.doi:10.1086/114146.
  4. ^abcdSchweitzer, 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.S2CID 102351979. A68.
  5. ^abcdefHoward, Andrew W.; et al. (2010). "The California Planet Survey. I. Four New Giant Exoplanets".The Astrophysical Journal.721 (2):1467–1481.arXiv:1003.3488.Bibcode:2010ApJ...721.1467H.doi:10.1088/0004-637X/721/2/1467.S2CID 14147776.
  6. ^Houdebine, Éric R.; et al. (2019)."The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs".The Astronomical Journal.158 (2): 56.arXiv:1905.07921.Bibcode:2019AJ....158...56H.doi:10.3847/1538-3881/ab23fe.S2CID 159041104.
  7. ^abHojjatpanah, S.; et al. (2019). "Catalog for the ESPRESSO blind radial velocity exoplanet survey".Astronomy & Astrophysics.629: A80.arXiv:1908.04627.Bibcode:2019A&A...629A..80H.doi:10.1051/0004-6361/201834729.S2CID 199552090.
  8. ^abRojas-Ayala, Bárbara; et al. (April 2012)."Metallicity and Temperature Indicators in M Dwarf K-band Spectra: Testing New and Updated Calibrations with Observations of 133 Solar Neighborhood M Dwarfs"(PDF).The Astrophysical Journal.748 (2): 93.arXiv:1112.4567.Bibcode:2012ApJ...748...93R.doi:10.1088/0004-637X/748/2/93.S2CID 41902340.Archived(PDF) from the original on 2021-01-29. Retrieved2018-11-04.
  9. ^Lindgren, Sara; Heiter, Ulrike (2017)."Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature".Astronomy and Astrophysics.604. A97.arXiv:1705.08785.Bibcode:2017A&A...604A..97L.doi:10.1051/0004-6361/201730715.S2CID 119216828.Archived from the original on 2021-01-23. Retrieved2018-09-03.
  10. ^abcdeVeyette, Mark J.; Muirhead, Philip S. (August 2018)."Chemo-kinematic Ages of Eccentric-planet-hosting M Dwarf Stars".The Astrophysical Journal.863 (2): 16.arXiv:1807.06017.Bibcode:2018ApJ...863..166V.doi:10.3847/1538-4357/aad40e.S2CID 119218351. 166.
  11. ^"Wolf 1539".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2021-11-17.
  12. ^Lépine, Sébastien; Shara, Michael M. (March 2005). "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)".The Astronomical Journal.129 (3):1483–1522.arXiv:astro-ph/0412070.Bibcode:2005AJ....129.1483L.doi:10.1086/427854.S2CID 2603568.
  13. ^abXiao, Guang-Yao; Liu, Yu-Juan; et al. (March 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements".Research in Astronomy and Astrophysics.23 (5).arXiv:2303.12409.Bibcode:2023RAA....23e5022X.doi:10.1088/1674-4527/accb7e.S2CID 257663647.
  14. ^Butler, R. Paul; et al. (13 April 2017)."The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey".The Astronomical Journal.153 (5): 208.arXiv:1702.03571.Bibcode:2017AJ....153..208B.doi:10.3847/1538-3881/aa66ca.hdl:2299/18220.S2CID 14954371.
  15. ^abTuomi, M.; Jones, H. R. A.; Anglada-Escudé, G.; Butler, R. P.; Arriagada, P.; Vogt, S. S.; et al. (2019). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood".arXiv:1906.04644 [astro-ph.EP].


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