Gliese 686
In today's world, Gliese 686 is a topic of great relevance and interest to a wide spectrum of people. From professionals to amateurs, Gliese 686 has captured the attention of millions around the world. Whether due to its impact on society, its relevance in the scientific field or its influence on popular culture, Gliese 686 has become a recurring topic in daily conversations, academic debates and the media. In this article, we will explore in depth the different aspects related to Gliese 686, analyzing its importance, its implications and its evolution over time. Join us on this journey to discover more about Gliese 686 and its impact on the world today!
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Hercules |
| Right ascension | 17h 37m 53.347s |
| Declination | +18° 35′ 30.16″ |
| Apparent magnitude (V) | 9.577 |
| Characteristics | |
| Spectral type | M1.0V |
| B−V color index | 1.530±0.015 |
| Astrometry | |
| Radial velocity (Rv) | −9.55±0.1 km/s |
| Proper motion (μ) | RA: 926.638 mas/yr Dec.: 984.455 mas/yr |
| Parallax (π) | 122.5546 ± 0.0176 mas |
| Distance | 26.613 ± 0.004 ly (8.160 ± 0.001 pc) |
| Absolute magnitude (MV) | 10.08 |
| Details | |
| Mass | 0.426±0.017 M☉ |
| Radius | 0.427±0.013 R☉ |
| Luminosity | 0.0295±0.0007 L☉ |
| Surface gravity (log g) | 4.87±0.07 cgs |
| Temperature | 3,656±51 K |
| Metallicity | −0.23±0.16 dex |
| Rotation | 38.732±0.286 d |
| Rotational velocity (v sin i) | 2.49 km/s |
| Other designations | |
| 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 26.6 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. It is orbiting close to the host star with a separation of 0.091 AU (13.6 Gm) and an orbital period of 15.5 days. Since the inclination of its orbit is unknown, only a lower bound on its mass can be determined: it has at least 6.6 times the mass of the planet Earth.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥6.624±0.432 M🜨 | 0.091±0.001 | 15.530±0.0011 | 0.050±0.030 | — | — |
References
- ^ a b c 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 119257644.
- ^ a b c d Vallenari, 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 at VizieR.
- ^ a b c d e 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.
- ^ a b c 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. (2021), "A Collage of Small Planets from the Lick–Carnegie Exoplanet Survey: Exploring the Super-Earth and Sub-Neptune Mass Regime", The Astronomical Journal, 161 (1): 10, arXiv:2011.08867, Bibcode:2021AJ....161...10B, doi:10.3847/1538-3881/abc2d0, S2CID 227013469
- ^ 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, Xavier; Delfosse, Xavier; Udry, Stéphane; Santos, Nuno C.; Forveille, Thierry; Ségransan, Damien (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): 635–642. arXiv:astro-ph/0503260. Bibcode:2005A&A...442..635B. doi:10.1051/0004-6361:20053046. S2CID 13900901.
