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{{Starbox observe |
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{{Starbox observe |
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| epoch = J2000 |
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| epoch = J2000 |
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| constell = ] |
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| constell = ]<ref name=Anderson_Francis_2012/> |
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| ra = {{RA|17|37|53.34674}}<ref name=GaiaDR2>{{cite DR2}}</ref> |
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| ra = {{RA|17|37|53.347}}<ref name=GaiaDR3/> |
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| dec = {{DEC|+18|35|30.1607}}<ref name=GaiaDR2/> |
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| dec = {{DEC|+18|35|30.16}}<ref name=GaiaDR3/> |
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| appmag_v = 9.577<ref name=Affer/> |
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| appmag_v = 9.577<ref name=Affer/> |
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}} |
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}} |
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{{Starbox character |
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{{Starbox character |
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| class = M1<ref name=Affer/> |
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| class = M1.0V<ref name=Burt2020/> |
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| b-v = 1.530{{±|0.015}}<ref name=Anderson_Francis_2012/> |
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| u-b = |
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| variable = |
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{{Starbox astrometry |
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{{Starbox astrometry |
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| radial_v = −9.55{{±|0.1}}<ref name=Nidever/> |
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| radial_v = −9.55 ± 0.1<ref name=Nidever>{{cite journal|bibcode=2002ApJS..141..503N|title=Radial Velocities for 889 Late-Type Stars|journal=The Astrophysical Journal Supplement Series|volume=141|issue=2|pages=503–522|last1=Nidever|first1=David L.|last2=Marcy|first2=Geoffrey W.|last3=Butler|first3=R. Paul|last4=Fischer|first4=Debra A.|last5=Vogt|first5=Steven S.|last6=McGahee|first6=C. E.|last7=O'Donoghue|first7=A. A.|last8=Knox|first8=E. R.|year=2002|arxiv=astro-ph/0112477|doi=10.1086/340570|s2cid=51814894}}</ref> |
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| prop_mo_ra = 926.741<ref name=GaiaDR2/> |
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| prop_mo_ra = 926.638 |
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| prop_mo_dec = 984.697<ref name=GaiaDR2/> |
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| prop_mo_dec = 984.455 |
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| pm_footnote = <ref name=GaiaDR3/> |
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| parallax = 122.5546 |
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| parallax = 122.5546 |
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| p_error = 0.0176 |
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| p_error = 0.0176 |
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| parallax_footnote = <ref name="GaiaEDR3">{{Cite Gaia EDR3|4550763526539955712}}</ref> |
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| parallax_footnote = <ref name=GaiaDR3/> |
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| absmag_v = 10.08<ref name=Anderson_Francis_2012/> |
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}} |
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}} |
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{{Starbox detail |
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{{Starbox detail |
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| source = <ref name=Affer/> |
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| source = <ref name=Burt2020/> |
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| mass = {{val|0.426|0.017}} |
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| temperature = 3663 ± 68 |
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| metal_fe = −0.30 ± 0.09 |
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| radius = {{val|0.427|0.013}} |
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| mass = 0.42 ± 0.05 |
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| luminosity = {{val|0.0295|0.0007}} |
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| radius = 0.42 ± 0.05 |
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| gravity = {{val|4.87|0.07}} |
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| temperature = {{val|3656|51|fmt=commas}} |
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| gravity = 4.83 ± 0.04 |
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| luminosity = 0.028 ± 0.006 |
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| metal_fe = {{val|−0.23|0.16}} |
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| rotation = {{val|38.732|0.286|ul=d}} |
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| rotational_velocity = 1.01 ± 0.80 |
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| rotational_velocity = 2.49 |
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{{Starbox catalog |
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{{Starbox catalog |
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{{Starbox end}} |
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'''Gliese 686''' (GJ 686 / HIP 86287 / LHS 452)<ref name="SIMBAD1">{{cite simbad|title=LHS 452|access-date=2019-09-02}}</ref> is a ] in the constellation of ], with an ] +9.577.<ref name=Affer/> Although it is close to the ] - at 26.5 ] - it is not the closest known star in its constellation, since ] is 20.9 light years away.<ref name="closeststars">{{cite web|url=http://www.closeststars.com/|website=closeststars.com|title=Closest stars|access-date=2019-03-31}}</ref> The closest system to this star is the bright ], at 4.5 light years. They are followed by ] and ], at 7.2 and 7.6 light years respectively.<ref name="ISDB">{{cite web|url=http://www.stellar-database.com/Scripts/find_neighbors.exe?ID=122400&ly=15|website=stellar-database.com|title=Stars within 15 light-years of Bonner Durchmusterung +18°3421 (The Internet Stellar Database)|access-date=2019-03-31}}</ref> |
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'''Gliese 686''' (GJ 686 / HIP 86287 / LHS 452)<ref name="SIMBAD1"/> is a ] in the constellation of ], with an ] +9.577.<ref name=Affer/> Although it is close to the ] – at 26.6 ]s – it is not the closest known star in its constellation, since ] is 20.9 light years away.<ref name="closeststars">{{cite web|url=http://www.closeststars.com/|website=closeststars.com|title=Closest stars|access-date=2019-03-31|archive-date=2023-04-11|archive-url=https://web.archive.org/web/20230411091505/http://www.closeststars.com/|url-status=live}}</ref> The closest system to this star is the bright ], at 4.5 light years. They are followed by ] and ], at 7.2 and 7.6 light years respectively.<ref name="ISDB">{{cite web|url=http://www.stellar-database.com/Scripts/find_neighbors.exe?ID=122400&ly=15|website=stellar-database.com|title=Stars within 15 light-years of Bonner Durchmusterung +18°3421 (The Internet Stellar Database)|access-date=2019-03-31}}</ref> |
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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. |
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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|archive-date=2023-04-11|archive-url=https://web.archive.org/web/20230411091504/http://www.stellar-database.com/Scripts/search_star.exe?Catalog=HIC&CatNo=86287|url-status=live}}</ref> while its total luminosity is equivalent to 2.7% that of the Sun,<ref name="Morales"/> 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: it is 6.5 times more luminous than ] and 15 times more than ], the closest star to the Solar System. |
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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 ]. |
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Gliese 686 has a radius approximately half ]. 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"/><ref name="Jenkins"/> It has an approximate mass between 45% and 49% of the solar mass<ref name="Bonfils"/> and is a star with characteristics comparable to that of ]. |
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== Planetary system == |
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== Planetary system == |
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Gliese 686 has one known ] planet detected by ].<ref name=Affer/> It is orbiting close to the host star with a separation of {{cvt|0.091|AU|Gm}} and an ] of 15.5 days. Since the ] 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. |
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Gliese 686 has one known ] planet detected by ].<ref name=Affer>{{Cite journal|last1=Affer|first1=L.|last2=Damasso|first2=M.|last3=Micela|first3=G.|last4=Poretti|first4=E.|last5=Scandariato|first5=G.|last6=Maldonado|first6=J.|last7=Lanza|first7=A. F.|last8=Covino|first8=E.|last9=Rubio|first9=A. Garrido|date=31 January 2019|title=HADES RV program with HARPS-N at TNG. IX. A super-Earth around the M dwarf Gl686|arxiv=1901.05338|journal=Astronomy & Astrophysics|volume=622|pages=A193|doi=10.1051/0004-6361/201834868|bibcode=2019A&A...622A.193A|s2cid=118863481|issn=0004-6361}}</ref> |
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{{OrbitboxPlanet begin}} |
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{{OrbitboxPlanet begin |
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| table_ref = <ref name=Burt2020/> |
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{{OrbitboxPlanet|exoplanet=] |
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}} |
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|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> |
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{{OrbitboxPlanet |
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|period=15.53209{{±|0.00166|0.00167}} |
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| exoplanet = b |
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|semimajor=0.091±0.004 |
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| mass_earth = {{val|6.624|0.432|p=≥}} |
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|eccentricity=}} |
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| period = {{val|15.530|0.0011}} |
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| semimajor = {{val|0.091|0.001}} |
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| eccentricity = {{val|0.050|0.030}} |
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{{Orbitbox end}} |
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==References== |
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==References== |
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{{reflist|30em}} |
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{{reflist|30em|refs= |
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<ref name="SIMBAD1">{{cite simbad|title=LHS 452|access-date=2019-09-02}}</ref> |
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<ref name=GaiaDR3>{{Cite Gaia DR3|4550763526539955712}}</ref> |
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<ref name=Nidever>{{cite journal|bibcode=2002ApJS..141..503N|title=Radial Velocities for 889 Late-Type Stars|journal=The Astrophysical Journal Supplement Series|volume=141|issue=2|pages=503–522|last1=Nidever|first1=David L.|last2=Marcy|first2=Geoffrey W.|last3=Butler|first3=R. Paul|last4=Fischer|first4=Debra A.|last5=Vogt|first5=Steven S.|last6=McGahee|first6=C. E.|last7=O'Donoghue|first7=A. A.|last8=Knox|first8=E. R.|year=2002|arxiv=astro-ph/0112477|doi=10.1086/340570|s2cid=51814894}}</ref> |
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<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> |
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<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|access-date=2019-03-31|archive-date=2018-10-02|archive-url=https://web.archive.org/web/20181002100426/http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2008A%26A...478..507M&db_key=AST&nosetcookie=1|url-status=live}}</ref> |
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<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> |
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<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> |
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<ref name=Anderson_Francis_2012>{{cite journal | last1=Anderson | first1=E. | last2=Francis | first2=Ch. | title=XHIP: An extended hipparcos compilation | journal=Astronomy Letters | volume=38 | issue=5 | pages=331 | year=2012 | bibcode=2012AstL...38..331A | arxiv=1108.4971 | doi=10.1134/S1063773712050015 | s2cid=119257644 }}</ref> |
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<ref name=Affer>{{Cite journal|last1=Affer|first1=L.|last2=Damasso|first2=M.|last3=Micela|first3=G.|last4=Poretti|first4=E.|last5=Scandariato|first5=G.|last6=Maldonado|first6=J.|last7=Lanza|first7=A. F.|last8=Covino|first8=E.|last9=Rubio|first9=A. Garrido|date=31 January 2019|title=HADES RV program with HARPS-N at TNG. IX. A super-Earth around the M dwarf Gl686|arxiv=1901.05338|journal=Astronomy & Astrophysics|volume=622|pages=A193|doi=10.1051/0004-6361/201834868|bibcode=2019A&A...622A.193A|s2cid=118863481|issn=0004-6361}}</ref> |
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<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 |doi-access=free }}</ref> |
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{{Stars of Hercules}} |
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{{Stars of Hercules}} |
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{{DEFAULTSORT:Gliese 686}} |
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{{DEFAULTSORT:Gliese 686}} |
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