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Gliese 686 (GJ 686 / HIP 86287 / LHS 452)  is a star in the Hercules constellation of apparent magnitude +9.62. 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 Of spectral type M1.0V, has an effective temperature of 3484 ± 50 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.

References

1. ^ LHS 452 - High proper-motion Star (SIMBAD)
2. Closest stars
3. Stars within 15 light-years of Bonner Durchmusterung +18°3421 (The Internet Stellar Database)
4. Bonner Durchmusterung +18°3421 (The Internet Stellar Database)
5. Morales, J. C.; Ribas, I.; Jordi, C. (2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics. 478 (2). pp. 507-512.{{cite journal}}: CS1 maint: multiple names: authors list (link)
6. ^ 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). pp. 1657-1673.
7. 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). pp. 975-988.{{cite journal}}: CS1 maint: multiple names: authors list (link)
8. 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.{{cite journal}}: CS1 maint: multiple names: authors list (link)
9. 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.

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