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Revision as of 13:19, 25 July 2020 by Rjwilmsi (talk | contribs) (10.1088/0004-637X/704/2/975)(diff) ← Previous revision | Latest revision (diff) | Newer revision → (diff) Star in the Hercules constellation| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Hercules |
| Right ascension | 17 37 53.34674 |
| Declination | +18° 35′ 30.1607″ |
| Apparent magnitude (V) | 9.577 |
| Characteristics | |
| Spectral type | M1 |
| Astrometry | |
| Radial velocity (Rv) | −9.55 ± 0.1 km/s |
| Proper motion (μ) | RA: 926.741 mas/yr Dec.: 984.697 mas/yr |
| Parallax (π) | 122.5609 ± 0.0346 mas |
| Distance | 26.612 ± 0.008 ly (8.159 ± 0.002 pc) |
| Details | |
| 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 | −0.30 ± 0.09 dex |
| Rotational velocity (v sin i) | 1.01 ± 0.80 km/s |
| Other designations | |
| BD+18 3421, HIP 86287, G 170-55, LHS 452 | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
Gliese 686 (GJ 686 / HIP 86287 / LHS 452) is a star in the constellation of Hercules, with an apparent magnitude +9.577. 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. 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.
Gliese 686 is one of the many red dwarfs in the Solar System neighborhood with a spectral type of M1V, and has an effective temperature of about 3600 K. Its brightness in the visible spectrum is equal to 0.82% of that of the Sun, while its total luminosity is equivalent to 2.7% that of the Sun, 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. It has a metallic content lower than that of the Sun; various studies estimate its index metallicity between -0.25 and -0.44. It has an approximate mass between 45% and 49% of the solar mass 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.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 7.1±0.9 M🜨 | 0.091±0.004 | 15.53209+0.00166−0.00167 | — | — | — |
References
- ^ 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.
- ^ 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. doi:10.1051/0004-6361/201834868. ISSN 0004-6361.
- 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.
- ^ "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. doi:10.1051/0004-6361:20078324. pp. 507-512.
- ^ 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). 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. Bibcode:2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975.
- 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). pp. 635-642.
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