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| Gliese 686 is one of the many ] in the Solar System neighborhood Of ] M1.0V,<ref name="SIMBAD1" /> has an ] of 3484 ± 50 ] . Its ] in the ] is equal to 0.82% of that of the ],<ref name="ISDB2"></ref> while its total luminosity is equivalent to 2.7% that of the Sun,<ref name="Morales">{{cita publicación|autor=Morales, J. C.; Ribas, I.; Jordi, C.|título=The effect of activity on stellar temperatures and radii|año=2008|publicación=]|volumen=478|número=2|id=pp. 507-512|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008A%26A...478..507M&db_key=AST&nosetcookie=1}}</ref> since a significant amount of the radiation emitted by these stars is ]. Considering only this last parameter, Gliese 686 is considerably brighter than other known red dwarfs; thus, it is 6.5 times more luminous than ] and 15 times more than ] , the closest star to the Solar System. | Gliese 686 is one of the many ] in the Solar System neighborhood Of ] M1.0V,<ref name="SIMBAD1" /> has an ] of 3484 ± 50 ] . Its ] in the ] is equal to 0.82% of that of the ],<ref name="ISDB2"></ref> while its total luminosity is equivalent to 2.7% that of the Sun,<ref name="Morales">{{cita publicación|autor=Morales, J. C.; Ribas, I.; Jordi, C.|título=The effect of activity on stellar temperatures and radii|año=2008|publicación=]|volumen=478|número=2|id=pp. 507-512|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008A%26A...478..507M&db_key=AST&nosetcookie=1}}</ref> since a significant amount of the radiation emitted by these stars is ]. Considering only this last parameter, Gliese 686 is considerably brighter than other known red dwarfs; thus, it is 6.5 times more luminous than ] and 15 times more than ] , the closest star to the Solar System. | ||
| Gliese 686 has a radius approximately equal to half the ]. Its projected ] is 2.5 km / s, its ] being equal to or less than 10.3 days.<ref name="Houdebine" /> It has a metallic content lower than that of the Sun; various studies estimate its index ] between -0.25 and -0.44.<ref name="Houdebine">{{cita publicación|autor=Houdebine, E. R.|título=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars|año=2010|publicación=]|volumen=407|número=3|id=pp. 1657-1673|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2010MNRAS.407.1657H&db_key=AST&nosetcookie=1}}</ref> |
Gliese 686 has a radius approximately equal to half the ]. Its projected ] is 2.5 km / s, its ] being equal to or less than 10.3 days.<ref name="Houdebine" /> It has a metallic content lower than that of the Sun; various studies estimate its index ] between -0.25 and -0.44.<ref name="Houdebine">{{cita publicación|autor=Houdebine, E. R.|título=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars|año=2010|publicación=]|volumen=407|número=3|id=pp. 1657-1673|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2010MNRAS.407.1657H&db_key=AST&nosetcookie=1}}</ref><ref name="Jenkins">{{cita publicación|autor=Jenkins, J. S.; Ramsey, L. W.; Jones, H. R. A.; Pavlenko, Y.; Gallardo, J.; Barnes, J. R.; Pinfield, D. J.|título=Rotational Velocities for M Dwarfs|año=2009|publicación=]|volumen=704|número=2|id=pp. 975-988|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2009ApJ...704..975J&db_key=AST&nosetcookie=1}}</ref> It has an approximate mass between 45% and 49% of the solar mass <ref name="Bonfils">{{cita publicación|autor=Bonfils, X.; Delfosse, X.; Udry, S.; Santos, N. C.; Forveille, T.; Ségransan, D.|título=Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence|año=2005|publicación=]|volumen=442|número=2|id=pp. 635-642|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2005A%26A...442..635B&db_key=AST&nosetcookie=1}}</ref> and is a star with characteristics comparable to that of ] . | ||
| == Planetary System == | == Planetary System == | ||
Revision as of 17:17, 31 March 2019
| Constellation | Hercules |
| Right ascension α | 17h 37min 53,35s |
| Declination δ | +18º 35’ 30,2’’ |
| Distance | 26,5 light years |
| Apparent Magnitude | +9,62 |
| Absolute Magnitude | +10,17 |
| Luminosity | 0,027 soles |
| Temperature | 3484 ± 50 K |
| Mass | 0,47 solar |
| Radius | 0,51 solar |
| Spectral type | M1.0V |
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.
| 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 | — | — | — |
- ^ LHS 452 - High proper-motion Star (SIMBAD)
- Closest stars
- Stars within 15 light-years of Bonner Durchmusterung +18°3421 (The Internet Stellar Database)
- Bonner Durchmusterung +18°3421 (The Internet Stellar Database)
- 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) - ^ 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.
- 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) - 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) - 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. doi:10.1051/0004-6361/201834868. ISSN 0004-6361.
- "HADES RV program with HARPS-N at the TNG IX. A super-Earth around the M dwarf Gl 686" (PDF). 31 Jan 2019.
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