Gliese 179

Last updated
Gliese 179
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Orion
Right ascension 04h 52m 05.73212s [1]
Declination +06° 28′ 35.5887″ [1]
Apparent magnitude  (V)11.94 [2]
Characteristics
Spectral type M2V [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−B color index 1.26 [2]
B−V color index 1.590±0.015 [2]
V−R color index 1.09 [2]
R−I color index 1.52 [2]
Astrometry
Radial velocity (Rv)–9.05±0.15 [2]  km/s
Proper motion (μ)RA: 153.615  mas/yr [1]
Dec.: −306.046  mas/yr [1]
Parallax (π)80.5623 ± 0.0236  mas [1]
Distance 40.48 ± 0.01  ly
(12.413 ± 0.004  pc)
Absolute magnitude  (MV)11.50 [2]
Details
Mass 0.400±0.005 M☉ [4]
0.357±0.03 [5]   M☉
Radius 0.400±0.005 R☉ [4]
0.318±0.024 R☉ [6]
0.38±0.02 [5]   R☉
Luminosity 0.0158±0.0003 L☉ [4]
0.016±0.02 [5]   L☉
Surface gravity (log g)4.148 [7]   cgs
Temperature 3,424±16 [8]   K
Metallicity [Fe/H]+0.36±0.04 dex [9]
+0.30±0.10 dex [5]
+0.12 [10]   dex
Age 4.6+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
SIMBAD data
Exoplanet Archive data
ARICNS data

Gliese 179 is a small red dwarf star with an exoplanetary companion in the equatorial constellation of Orion. It is much too faint to be visible to the naked eye with an apparent visual magnitude of 11.94. [2] The system is located at a distance of 40.5 light-years (12.4 parsecs ) from the Sun based on parallax measurements, but is drifting closer with a radial velocity of –9 km/s. [2] It is a high proper motion star, traversing the celestial sphere at an angular rate of 0.370″ ·yr−1. [12]

This is an M-type main-sequence star with a stellar 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 is chromospherically active [5] with a projected rotational velocity of 4 km/s. [7] This star is smaller and less massive than the Sun, but has a higher metal content. It is radiating just 1.6% of the luminosity of the Sun from its photosphere at an effective temperature of 3,424. [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 via astrometry. [13] A second candidate planet was reported in 2017 [14] and was also reported in a 2019 preprint. 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)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
c(unconfirmed)≥4.9±2.7 M🜨 0.032±0.0033.4798+0.0014
−0.0010		0.04+0.27
−0.04		——
b 0.95+0.16
−0.11  MJ 		2.424+0.071
−0.075		2303+34
−31		0.179+0.048
−0.044		61+16
−13 or 119+13
−16 ° 		—

See also

Related Research Articles

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Gliese 849, or GJ 849, is a small, solitary star in the equatorial constellation of Aquarius. It has a reddish hue and is invisible to the naked eye with an apparent visual magnitude of 10.41. The distance to this star is 28.8 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.3 km/s. It has a pair of confirmed gas giant companions.

<span class="mw-page-title-main">HD 136118</span> Star in the constellation Serpens

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References

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  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 Anderson, 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.
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  5. 1 2 3 4 5 6 Howard, 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. 1 2 Hojjatpanah, 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. 1 2 Rojas-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.
  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.
  10. 1 2 3 4 5 Veyette, 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 . Retrieved 2021-11-17.
  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. 1 2 Xiao, 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. 1 2 Tuomi, 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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