Gliese 686: Difference between revisions

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	Gliese 686 is one of the many ] in the Solar System neighborhood with a ] of M1V,<ref name=Affer/><ref name="SIMBAD1" /> and has an ] of about 3600 ].<ref name=Affer/> Its ] in the ] is equal to 0.82% of that of the ],<ref name="ISDB2">{{cite web\|url=http://www.stellar-database.com/Scripts/search_star.exe?Catalog=HIC&CatNo=86287\|website=stellar-database.com\|title=Bonner Durchmusterung +18°3421 (The Internet Stellar Database)\|access-date=2019-03-31}}</ref> while its total luminosity is equivalent to 2.7% that of the Sun,<ref name="Morales">{{cite journal\|author1=Morales, J. C.\|author2=Ribas, I.\|author3=Jordi, C.\|title=The effect of activity on stellar temperatures and radii\|year=2008\|journal=]\|volume=478\|issue=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\|arxiv=0711.3523\|doi=10.1051/0004-6361:20078324\|pages=507–512\|bibcode=2008A&A...478..507M\|s2cid=16238033}}</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 with a ] of M1V,<ref name=Affer/><ref name="SIMBAD1" /> and has an ] of about 3600 ].<ref name=Affer/> Its ] in the ] is equal to 0.82% of that of the ],<ref name="ISDB2">{{cite web\|url=http://www.stellar-database.com/Scripts/search_star.exe?Catalog=HIC&CatNo=86287\|website=stellar-database.com\|title=Bonner Durchmusterung +18°3421 (The Internet Stellar Database)\|access-date=2019-03-31}}</ref> while its total luminosity is equivalent to 2.7% that of the Sun,<ref name="Morales">{{cite journal\|author1=Morales, J. C.\|author2=Ribas, I.\|author3=Jordi, C.\|title=The effect of activity on stellar temperatures and radii\|year=2008\|journal=]\|volume=478\|issue=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\|arxiv=0711.3523\|doi=10.1051/0004-6361:20078324\|pages=507–512\|bibcode=2008A&A...478..507M\|s2cid=16238033}}</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">{{cite journal\|author=Houdebine, E. R.\|title=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars\|year=2010\|journal=]\|volume=407\|issue=3\|page=1657\|id=pp. 1657–1673\|doi= 10.1111/j.1365-2966.2010.16827.x\|bibcode=2010MNRAS.407.1657H\|doi-access=free}}</ref><ref name="Jenkins">{{cite journal\|author1=Jenkins, J. S.\|author2=Ramsey, L. W.\|author3=Jones, H. R. A.\|author4=Pavlenko, Y.\|author5=Gallardo, J.\|author6=Barnes, J. R.\|author7=Pinfield, D. J.\|title=Rotational Velocities for M Dwarfs\|year=2009\|journal=]\|volume=704\|issue=2\|pages=975–988\|doi=10.1088/0004-637X/704/2/975\|bibcode=2009ApJ...704..975J\|arxiv=0908.4092\|s2cid=119203469}}</ref> It has an approximate mass between 45% and 49% of the solar mass <ref name="Bonfils">{{cite journal \|doi=10.1051/0004-6361:20053046 \|last1=Bonfils \|first1=Xavier \|last2=Delfosse \|first2=Xavier\|last3=Udry \|first3=Stéphane \|last4=Santos \|first4=Nuno C. \|last5=Forveille \|first5=Thierry \|last6=Ségransan \|first6=Damien \|title=Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence \|year=2005 \|journal=] \|volume=442 \|issue=2 \|arxiv=astro-ph/0503260 \|bibcode=2005A&A...442..635B \|s2cid=13900901 \|pages=~~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 ].		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">{{cite journal\|author=Houdebine, E. R.\|title=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars\|year=2010\|journal=]\|volume=407\|issue=3\|page=1657\|id=pp. 1657–1673\|doi= 10.1111/j.1365-2966.2010.16827.x\|bibcode=2010MNRAS.407.1657H\|doi-access=free}}</ref><ref name="Jenkins">{{cite journal\|author1=Jenkins, J. S.\|author2=Ramsey, L. W.\|author3=Jones, H. R. A.\|author4=Pavlenko, Y.\|author5=Gallardo, J.\|author6=Barnes, J. R.\|author7=Pinfield, D. J.\|title=Rotational Velocities for M Dwarfs\|year=2009\|journal=]\|volume=704\|issue=2\|pages=975–988\|doi=10.1088/0004-637X/704/2/975\|bibcode=2009ApJ...704..975J\|arxiv=0908.4092\|s2cid=119203469}}</ref> It has an approximate mass between 45% and 49% of the solar mass <ref name="Bonfils">{{cite journal \|doi=10.1051/0004-6361:20053046 \|last1=Bonfils \|first1=Xavier \|last2=Delfosse \|first2=Xavier\|last3=Udry \|first3=Stéphane \|last4=Santos \|first4=Nuno C. \|last5=Forveille \|first5=Thierry \|last6=Ségransan \|first6=Damien \|title=Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence \|year=2005 \|journal=] \|volume=442 \|issue=2 \|arxiv=astro-ph/0503260 \|bibcode=2005A&A...442..635B \|s2cid=13900901 \|pages=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 ==
Line 50:		Line 50:
	{{OrbitboxPlanet begin}}		{{OrbitboxPlanet begin}}
	{{OrbitboxPlanet\|exoplanet=]		{{OrbitboxPlanet\|exoplanet=]
	\|mass_earth=>6.624{{±\|0.432}}<ref name=Burt2020>{{citation\|arxiv=2011.08867\|title=A Collage of Small Planets from the Lick–Carnegie Exoplanet Survey: Exploring the Super-Earth and Sub-Neptune Mass Regime\|year=2021\|last1=Burt\|first1=Jennifer A.\|last2=Feng\|first2=Fabo\|last3=Holden\|first3=Bradford\|last4=Mamajek\|first4=Eric E.\|last5=Huang\|first5=Chelsea X.\|last6=Rosenthal\|first6=Mickey M.\|last7=Wang\|first7=Songhu\|last8=Paul Butler\|first8=R.\|last9=Vogt\|first9=Steven S.\|last10=Laughlin\|first10=Gregory\|last11=Henry\|first11=Gregory W.\|last12=Teske\|first12=Johanna K.\|last13=Wang\|first13=Sharon W.\|last14=Crane\|first14=Jeffrey D.\|last15=Shectman\|first15=Steve A.\|journal=The Astronomical Journal\|volume=161\|page=10\|doi=10.3847/1538-3881/abc2d0\|s2cid=227013469}}</ref>		\|mass_earth=>6.624{{±\|0.432}}<ref name=Burt2020>{{citation\|arxiv=2011.08867\|title=A Collage of Small Planets from the Lick–Carnegie Exoplanet Survey: Exploring the Super-Earth and Sub-Neptune Mass Regime\|year=2021\|last1=Burt\|first1=Jennifer A.\|last2=Feng\|first2=Fabo\|last3=Holden\|first3=Bradford\|last4=Mamajek\|first4=Eric E.\|last5=Huang\|first5=Chelsea X.\|last6=Rosenthal\|first6=Mickey M.\|last7=Wang\|first7=Songhu\|last8=Paul Butler\|first8=R.\|last9=Vogt\|first9=Steven S.\|last10=Laughlin\|first10=Gregory\|last11=Henry\|first11=Gregory W.\|last12=Teske\|first12=Johanna K.\|last13=Wang\|first13=Sharon W.\|last14=Crane\|first14=Jeffrey D.\|last15=Shectman\|first15=Steve A.\|journal=The Astronomical Journal\|volume=161\|issue=1 \|page=10\|doi=10.3847/1538-3881/abc2d0\|bibcode=2021AJ....161...10B \|s2cid=227013469}}</ref>
	\|period=15.53209{{±\|0.00166\|0.00167}}		\|period=15.53209{{±\|0.00166\|0.00167}}
	\|semimajor=0.091±0.004		\|semimajor=0.091±0.004

Revision as of 21:58, 24 February 2023

Star in the Hercules constellation

Gliese 686
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 (R_v)	−9.55 ± 0.1 km/s
Proper motion (μ)	RA: 926.741 mas/yr Dec.: 984.697 mas/yr
Parallax (π)	122.5546 ± 0.0176 mas
Distance	26.613 ± 0.004 ly (8.160 ± 0.001 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, 2MASS J17375330+1835295
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.

The Gliese 686 planetary system
Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (days)	Eccentricity	Inclination	Radius
b	>6.624±0.432 M_🜨	0.091±0.004	15.53209 _−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. 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.
Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
^ "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.
^ 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.
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{{citation}}: CS1 maint: unflagged free DOI (link)

Constellation of Hercules

Stars

Bayer	α (Rasalgethi) β (Kornephoros) γ δ (Sarin) ε ζ η θ ι κ (Marsic) λ (Maasym) μ ν ξ ο π ρ σ τ υ φ χ ψ ψ ω (Cujam)
Flamsteed	14 29 (h) 30 (g) 42 45 (l) 52 60 68 (u) 69 (e) 72 (w) 89 93 98 99 (b) 102 104 (A) 106 109 110 111 112 32 Oph
Variable	X AC AM BL DI DQ V446 V533 V772 V777 V838 V1674
HR	6669 6697 6806
HD	146389 (Irena) 147506 (Hunor) 149026 (Ogma) 152843 154345 155358 156668 159062 164595 164922
Other	BD +17° 3248 Furuhjelm 46 GD 362 Gliese 623 Gliese 638 Gliese 649 Gliese 686 GJ 3991 HAT-P-14 (Franz) HAT-P-18 HAT-P-67 Hercules X-1 GSC 02620-00648 Ross 640 TOI-2119 TrES-3 (Pipoltr) TYC 1031-1262-1 WASP-103 WISE 1738+2732 WISE 1741+2553

Exoplanets	14 Herculis b c HAT-P-14b (Sissi) HD 149026 b (Smertrios) HD 164922 b c WASP-103b

Star clusters	Messier 13 Messier 92 NGC 6229 Palomar 14

Nebulae	Abell 39 NGC 6210

Galaxies

NGC	6028 6039 6040 6041 6042 6043 6044 6045 6046 6047 6052 6053 6054 6055 6056 6057 6061 6078 6158 6166 6181 6207 6212 6239 6261 6263 6308 6452 6560
Other	1ES 1741+196 2MASX J16270254+4328340 3C 345 3C 346 A2261-BCG Arp 272 (NGC 6050 and IC 1179) AT2018cow IC 1182 IC 1189 Hercules Dwarf Hercules A IC 1192 IC 4617 Markarian 501 MCG+07-33-027 PGC 2046648 QSR J1819+3845 RX J1633.3+4718 UGC 11105

Galaxy clusters	Abell 2152 Abell 2199 Hercules Cluster Hercules Superclusters Zwicky's Triplet

Astronomical events	LBG-2377

Revision as of 15:57, 30 January 2023 editGraham87 (talk \| contribs)Account creators, Autopatrolled, Event coordinators, Extended confirmed users, Page movers, Importers, Rollbackers291,914 editsm Reverted edits by Shanaya Chaturvedi (talk) to last version by LoookeTag: Rollback ← Previous edit		Revision as of 21:58, 24 February 2023 edit undoCitation bot (talk \| contribs)Bots5,445,340 edits Alter: pages. Add: bibcode, issue. Formatted dashes. \| Use this bot. Report bugs. \| Suggested by Whoop whoop pull up \| #UCB_webform 2402/3626Next edit →
Line 42:		Line 42:
	Gliese 686 is one of the many ] in the Solar System neighborhood with a ] of M1V,<ref name=Affer/><ref name="SIMBAD1" /> and has an ] of about 3600 ].<ref name=Affer/> Its ] in the ] is equal to 0.82% of that of the ],<ref name="ISDB2">{{cite web\|url=http://www.stellar-database.com/Scripts/search_star.exe?Catalog=HIC&CatNo=86287\|website=stellar-database.com\|title=Bonner Durchmusterung +18°3421 (The Internet Stellar Database)\|access-date=2019-03-31}}</ref> while its total luminosity is equivalent to 2.7% that of the Sun,<ref name="Morales">{{cite journal\|author1=Morales, J. C.\|author2=Ribas, I.\|author3=Jordi, C.\|title=The effect of activity on stellar temperatures and radii\|year=2008\|journal=]\|volume=478\|issue=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\|arxiv=0711.3523\|doi=10.1051/0004-6361:20078324\|pages=507–512\|bibcode=2008A&A...478..507M\|s2cid=16238033}}</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 with a ] of M1V,<ref name=Affer/><ref name="SIMBAD1" /> and has an ] of about 3600 ].<ref name=Affer/> Its ] in the ] is equal to 0.82% of that of the ],<ref name="ISDB2">{{cite web\|url=http://www.stellar-database.com/Scripts/search_star.exe?Catalog=HIC&CatNo=86287\|website=stellar-database.com\|title=Bonner Durchmusterung +18°3421 (The Internet Stellar Database)\|access-date=2019-03-31}}</ref> while its total luminosity is equivalent to 2.7% that of the Sun,<ref name="Morales">{{cite journal\|author1=Morales, J. C.\|author2=Ribas, I.\|author3=Jordi, C.\|title=The effect of activity on stellar temperatures and radii\|year=2008\|journal=]\|volume=478\|issue=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\|arxiv=0711.3523\|doi=10.1051/0004-6361:20078324\|pages=507–512\|bibcode=2008A&A...478..507M\|s2cid=16238033}}</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">{{cite journal\|author=Houdebine, E. R.\|title=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars\|year=2010\|journal=]\|volume=407\|issue=3\|page=1657\|id=pp. 1657–1673\|doi= 10.1111/j.1365-2966.2010.16827.x\|bibcode=2010MNRAS.407.1657H\|doi-access=free}}</ref><ref name="Jenkins">{{cite journal\|author1=Jenkins, J. S.\|author2=Ramsey, L. W.\|author3=Jones, H. R. A.\|author4=Pavlenko, Y.\|author5=Gallardo, J.\|author6=Barnes, J. R.\|author7=Pinfield, D. J.\|title=Rotational Velocities for M Dwarfs\|year=2009\|journal=]\|volume=704\|issue=2\|pages=975–988\|doi=10.1088/0004-637X/704/2/975\|bibcode=2009ApJ...704..975J\|arxiv=0908.4092\|s2cid=119203469}}</ref> It has an approximate mass between 45% and 49% of the solar mass <ref name="Bonfils">{{cite journal \|doi=10.1051/0004-6361:20053046 \|last1=Bonfils \|first1=Xavier \|last2=Delfosse \|first2=Xavier\|last3=Udry \|first3=Stéphane \|last4=Santos \|first4=Nuno C. \|last5=Forveille \|first5=Thierry \|last6=Ségransan \|first6=Damien \|title=Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence \|year=2005 \|journal=] \|volume=442 \|issue=2 \|arxiv=astro-ph/0503260 \|bibcode=2005A&A...442..635B \|s2cid=13900901 \|pages=~~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 ].		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">{{cite journal\|author=Houdebine, E. R.\|title=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars\|year=2010\|journal=]\|volume=407\|issue=3\|page=1657\|id=pp. 1657–1673\|doi= 10.1111/j.1365-2966.2010.16827.x\|bibcode=2010MNRAS.407.1657H\|doi-access=free}}</ref><ref name="Jenkins">{{cite journal\|author1=Jenkins, J. S.\|author2=Ramsey, L. W.\|author3=Jones, H. R. A.\|author4=Pavlenko, Y.\|author5=Gallardo, J.\|author6=Barnes, J. R.\|author7=Pinfield, D. J.\|title=Rotational Velocities for M Dwarfs\|year=2009\|journal=]\|volume=704\|issue=2\|pages=975–988\|doi=10.1088/0004-637X/704/2/975\|bibcode=2009ApJ...704..975J\|arxiv=0908.4092\|s2cid=119203469}}</ref> It has an approximate mass between 45% and 49% of the solar mass <ref name="Bonfils">{{cite journal \|doi=10.1051/0004-6361:20053046 \|last1=Bonfils \|first1=Xavier \|last2=Delfosse \|first2=Xavier\|last3=Udry \|first3=Stéphane \|last4=Santos \|first4=Nuno C. \|last5=Forveille \|first5=Thierry \|last6=Ségransan \|first6=Damien \|title=Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence \|year=2005 \|journal=] \|volume=442 \|issue=2 \|arxiv=astro-ph/0503260 \|bibcode=2005A&A...442..635B \|s2cid=13900901 \|pages=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 ==
Line 50:		Line 50:
	{{OrbitboxPlanet begin}}		{{OrbitboxPlanet begin}}
	{{OrbitboxPlanet\|exoplanet=]		{{OrbitboxPlanet\|exoplanet=]
	\|mass_earth=>6.624{{±\|0.432}}<ref name=Burt2020>{{citation\|arxiv=2011.08867\|title=A Collage of Small Planets from the Lick–Carnegie Exoplanet Survey: Exploring the Super-Earth and Sub-Neptune Mass Regime\|year=2021\|last1=Burt\|first1=Jennifer A.\|last2=Feng\|first2=Fabo\|last3=Holden\|first3=Bradford\|last4=Mamajek\|first4=Eric E.\|last5=Huang\|first5=Chelsea X.\|last6=Rosenthal\|first6=Mickey M.\|last7=Wang\|first7=Songhu\|last8=Paul Butler\|first8=R.\|last9=Vogt\|first9=Steven S.\|last10=Laughlin\|first10=Gregory\|last11=Henry\|first11=Gregory W.\|last12=Teske\|first12=Johanna K.\|last13=Wang\|first13=Sharon W.\|last14=Crane\|first14=Jeffrey D.\|last15=Shectman\|first15=Steve A.\|journal=The Astronomical Journal\|volume=161\|page=10\|doi=10.3847/1538-3881/abc2d0\|s2cid=227013469}}</ref>		\|mass_earth=>6.624{{±\|0.432}}<ref name=Burt2020>{{citation\|arxiv=2011.08867\|title=A Collage of Small Planets from the Lick–Carnegie Exoplanet Survey: Exploring the Super-Earth and Sub-Neptune Mass Regime\|year=2021\|last1=Burt\|first1=Jennifer A.\|last2=Feng\|first2=Fabo\|last3=Holden\|first3=Bradford\|last4=Mamajek\|first4=Eric E.\|last5=Huang\|first5=Chelsea X.\|last6=Rosenthal\|first6=Mickey M.\|last7=Wang\|first7=Songhu\|last8=Paul Butler\|first8=R.\|last9=Vogt\|first9=Steven S.\|last10=Laughlin\|first10=Gregory\|last11=Henry\|first11=Gregory W.\|last12=Teske\|first12=Johanna K.\|last13=Wang\|first13=Sharon W.\|last14=Crane\|first14=Jeffrey D.\|last15=Shectman\|first15=Steve A.\|journal=The Astronomical Journal\|volume=161\|issue=1 \|page=10\|doi=10.3847/1538-3881/abc2d0\|bibcode=2021AJ....161...10B \|s2cid=227013469}}</ref>
	\|period=15.53209{{±\|0.00166\|0.00167}}		\|period=15.53209{{±\|0.00166\|0.00167}}
	\|semimajor=0.091±0.004		\|semimajor=0.091±0.004