Gliese 686
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Hercules |
| Right ascension | 17h 37m 53.34674s[1] |
| Declination | +18° 35′ 30.1607″[1] |
| Apparent magnitude (V) | 9.577[2] |
| Characteristics | |
| Spectral type | M1[2] |
| Astrometry | |
| Radial velocity (Rv) | −9.55 ± 0.1[3] km/s |
| Proper motion (μ) | RA: 926.741[1] mas/yr Dec.: 984.697[1] mas/yr |
| Parallax (π) | 122.5609 ± 0.0346 mas[1] |
| Distance | 26.612 ± 0.008 ly (8.159 ± 0.002 pc) |
| Details[2] | |
| Mass | 0.42 ± 0.05 M☉ |
| Radius | 0.42 ± 0.05 R☉ |
| Luminosity | 0.028 ± 0.006 L☉ |
| Surface gravity (log g) | 4.83 ± 0.04 cgs |
| Temperature | 3663 ± 68 K |
| Metallicity [Fe/H] | −0.30 ± 0.09 dex |
| Rotational velocity (v sin i) | 1.01 ± 0.80 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
Gliese 686 (GJ 686 / HIP 86287 / LHS 452)[4] is a star in the constellation of Hercules, with an apparent magnitude +9.577.[2] Although it is close to the Solar System - at 26.5 light years - it is not the closest known star in its constellation, since Gliese 661 is 20.9 light years away.[5] The closest system to this star is the bright μ Herculis, at 4.5 light years. They are followed by GJ 1230 and Gliese 673, at 7.2 and 7.6 light years respectively.[6]
Gliese 686 is one of the many red dwarfs in the Solar System neighborhood with a spectral type of M1V,[2][4] and has an effective temperature of about 3600 K.[2] Its brightness in the visible spectrum is equal to 0.82% of that of the Sun,[7] while its total luminosity is equivalent to 2.7% that of the Sun,[8] since a significant amount of the radiation emitted by these stars is infrared invisible light. Considering only this last parameter, Gliese 686 is considerably brighter than other known red dwarfs; thus, it is 6.5 times more luminous than Ross 154 and 15 times more than Proxima Centauri, the closest star to the Solar System.
Gliese 686 has a radius approximately equal to half the solar radius. Its projected rotation speed is 2.5 km / s, its rotation period being equal to or less than 10.3 days.[9] It has a metallic content lower than that of the Sun; various studies estimate its index metallicity between -0.25 and -0.44.[9][10] It has an approximate mass between 45% and 49% of the solar mass [11] and is a star with characteristics comparable to that of Lacaille 9352.
Planetary system
Gliese 686 has one known super-Earth planet detected by radial velocity.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >6.624±0.432[12] M🜨 | 0.091±0.004 | 15.53209+0.00166 −0.00167 |
— | — | — |
References
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data 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.
- ^ a b c d e f g Affer, L.; Damasso, M.; Micela, G.; Poretti, E.; Scandariato, G.; Maldonado, J.; Lanza, A. F.; Covino, E.; Rubio, A. Garrido (31 January 2019). "HADES RV program with HARPS-N at TNG. IX. A super-Earth around the M dwarf Gl686". Astronomy & Astrophysics. 622: A193. arXiv:1901.05338. Bibcode:2019A&A...622A.193A. doi:10.1051/0004-6361/201834868. ISSN 0004-6361. S2CID 118863481.
- ^ Nidever, David L.; Marcy, Geoffrey W.; Butler, R. Paul; Fischer, Debra A.; Vogt, Steven S.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2002). "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. S2CID 51814894.
- ^ a b c "LHS 452". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-02.
- ^ "Closest stars". closeststars.com. Retrieved 2019-03-31.
- ^ "Stars within 15 light-years of Bonner Durchmusterung +18°3421 (The Internet Stellar Database)". stellar-database.com. Retrieved 2019-03-31.
- ^ "Bonner Durchmusterung +18°3421 (The Internet Stellar Database)". stellar-database.com. Retrieved 2019-03-31.
- ^ Morales, J. C.; Ribas, I.; Jordi, C. (2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics. 478 (2): 507–512. arXiv:0711.3523. Bibcode:2008A&A...478..507M. doi:10.1051/0004-6361:20078324. S2CID 16238033. pp. 507-512.
- ^ a b Houdebine, E. R. (2010). "Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars". Monthly Notices of the Royal Astronomical Society. 407 (3): 1657. Bibcode:2010MNRAS.407.1657H. doi:10.1111/j.1365-2966.2010.16827.x. pp. 1657–1673.
- ^ Jenkins, J. S.; Ramsey, L. W.; Jones, H. R. A.; Pavlenko, Y.; Gallardo, J.; Barnes, J. R.; Pinfield, D. J. (2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal. 704 (2): 975–988. arXiv:0908.4092. Bibcode:2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975. S2CID 119203469.
- ^ Bonfils, X.; Delfosse, X.; Udry, S.; Santos, N. C.; Forveille, T.; Ségransan, D. (2005). "Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence". Astronomy and Astrophysics. 442 (2): 635. arXiv:astro-ph/0503260. Bibcode:2005A&A...442..635B. doi:10.1051/0004-6361:20053046. S2CID 13900901. pp. 635-642.
- ^ Burt, Jennifer A.; Feng, Fabo; Holden, Bradford; Mamajek, Eric E.; Huang, Chelsea X.; Rosenthal, Mickey M.; Wang, Songhu; Paul Butler, R.; Vogt, Steven S.; Laughlin, Gregory; Henry, Gregory W.; Teske, Johanna K.; Wang, Sharon W.; Crane, Jeffrey D.; Shectman, Steve A. (2020), A collage of small planets from the Lick Carnegie Exoplanet Survey :Exploring the super-Earth and sub-Neptune mass regime, arXiv:2011.08867
