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| {{Starbox begin
| | I'm Tamara and I live in Wroclaw. <br>I'm interested in Neuroscience, Magic and Arabic art. I like to travel and reading fantasy.<br><br>Here is my weblog - [http://www.6nest.com/space.php?uid=388598&do=blog&id=802563 How to get free fifa 15 coins] |
| | name = Gliese 710
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| }}
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| {{Starbox observe
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| | epoch = J2000
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| | ra = {{RA|18|19|50.84215}}<ref name=aaa474_2_653/>
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| | dec = {{DEC|–01|56|18.9841}}<ref name=aaa474_2_653/>
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| | appmag_v = 9.69<ref name="SIMBAD-Gliese710"/> (9.65–9.69)<ref name=gcvs71/>
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| | constell = [[Serpens]]
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| }}
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| {{Starbox character
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| | class = K7 Vk<ref name=aj132_1_161/>
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| | b-v = +1.36<ref name="SIMBAD-Gliese710"/>
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| | u-b = +1.23<ref name="SIMBAD-Gliese710"/>
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| | variable = Suspected<ref name=gcvs71/>
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| }}
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| {{Starbox astrometry
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| | radial_v = –13.8<ref name="Bobylev:arXiv1003.2160"/>
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| | prop_mo_ra = +1.15<ref name=aaa474_2_653/>
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| | prop_mo_dec = +1.99<ref name=aaa474_2_653/>
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| | parallax = 51.12
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| | p_error = 1.63
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| | parallax_error =<ref name=aaa474_2_653/><ref name="SIMBAD-Gliese710"/>
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| | absmag_v = 8.23 (8.19-8.23)<ref name=absolute_magnitude group=note/>{{Citation needed|date=January 2012}}
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| }}
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| {{Starbox detail
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| | mass = 0.6<ref name="García-Sánchez1999"/>
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| | radius = 0.67<ref name="Johnson"/>
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| | luminosity_bolometric = 0.084{{#tag:ref|Using the absolute visual magnitude of Gliese 710 <math>\scriptstyle M_{V_{\ast}}=8.23</math> with a [[bolometric correction]] of <math>\scriptstyle BC=-0.814</math><ref name="bolometric_correction"/> the bolometric magnitude can be calculated as <math>\scriptstyle M_{bol_{\ast}}=7.416</math>, the bolometric magnitude of the Sun <math>\scriptstyle M_{bol_{\odot}}=4.73</math>,<ref name="tableprovisoBC"/> therefore the bolometric luminosity can be calculated by <math>\scriptstyle \frac{L_{bol_{\ast}}}{L_{bol_{\odot}}}=10^{0.4\left(M_{bol_{\odot}} - M_{bol_{\ast}}\right)}</math>|group="note"|name=luminosity_bolometric}}{{Citation needed|date=January 2012}}
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| | luminosity_visual = 0.044<ref name=luminosity_visual group=note/>
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| | temperature = 4,250<ref name="García-Sánchez1999"/>
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| | metal =
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| | rotational_velocity = {{nowrap|6.42 ± 0.78}}<ref name=aaa514_A97/>
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| | age=
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| }}
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| {{Starbox catalog
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| | names=GJ 710, Gl 710, [[Bonner Durchmusterung|BD]]-01 3474, [[Hipparcos catalogue|HIP]] 89825, [[Henry Draper catalogue|HD]] 168442, U449, Vys/McC 63, NSV 10635<ref name="SIMBAD-Gliese710"/>
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| }}
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| {{Starbox end}}
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| '''Gliese 710''' is a [[star]] in the [[constellation]] [[Serpens Cauda]] with an [[apparent visual magnitude]] of 9.69. It has a [[stellar classification]] of K7 Vk,<ref name=aj132_1_161/> which means it is a [[main sequence]] star that is generating energy through the [[thermonuclear fusion]] of hydrogen at its core. (The suffix 'k' indicates that the spectrum shows absorption lines from interstellar matter.) The mass of this star is about 60%<ref name="García-Sánchez1999"/> of the [[solar mass|Sun's mass]] and it has an estimated 67% of the [[solar radius|Sun's radius]].<ref name="Johnson"/> It is a suspected [[variable star]] that may vary in magnitude from 9.65–9.69.
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| This star is currently about {{Convert|63.8|ly|pc|abbr=off|lk=on}} from [[Earth]], but its [[proper motion]], distance, and [[radial velocity]]<ref>See also: [[Stellar kinematics]].</ref> indicate that it will approach within a very small distance—perhaps under one light year—from the [[Sun]] within 1.4 million years, based on past and current ''[[Hipparcos]]'' data.<ref name="Bobylev:arXiv1003.2160" /> At closest approach it will be a first-magnitude star about as bright as [[Antares]]. The proper motion of Gliese 710 is very small for its distance, meaning it is traveling nearly directly in our line of sight.
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| In a time interval of ±10 million years from the present, Gliese 710 is the star whose combination of mass and close approach distance will cause the greatest [[gravitation]]al perturbation of the [[Solar System]].
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| == Computing and details of the closest approach ==
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| Gliese 710 has the potential to [[Perturbation (astronomy)|perturb]] the hypothetical [[Oort cloud]] enough to send a shower of [[comet]]s into the inner Solar System, possibly causing an [[impact event]]. However, dynamic models by García-Sánchez, et al. in 1999 indicate that the net increase in cratering rate due to the passage of Gliese 710 will be no more than 5%.<ref name="García-Sánchez1999"/> They estimate that the closest approach will happen in 1,360,000 years when the star will approach within 0.337 ± 0.177 [[parsec]]s (1.1 light-years) of the Sun.<ref name="García-Sánchez2001">{{cite journal
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| |last=García-Sánchez |first=J.
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| |coauthors=Weissman, P. R.; Preston, R. A.; Jones, D. L.; Lestrade, J.-F.; Latham, D. W.; Stefanik, R. P.; Paredes, J. M.
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| |title=Stellar encounters with the solar system
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| |journal=Astronomy and Astrophysics
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| |year=2001 |volume=379
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| |issue=2 |pages=634–659
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| |bibcode=2001A&A...379..634G
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| |doi=10.1051/0004-6361:20011330}}</ref>
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| [[Image:Kuiper oort.jpg|thumb|left|An artist's rendering of the [[Oort cloud]] and the [[Kuiper belt]] (inset)]]
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| More recent calculations by Bobylev in 2010 suggest Gliese 710 has an 86% chance of passing through the Oort cloud, considering the Oort cloud to be a spheroid around the Sun with semiminor and semimajor axes of 80,000 and 100,000 [[astronomical unit]]s. The distance of closest approach of Gliese 710 is difficult to compute precisely as it depends sensitively on its current position and velocity; Bobylev estimates that it will pass within 0.311 ± 0.167 pc (1.01 ± 0.54 light years) of the Sun.<ref name="Bobylev:arXiv1003.2160">{{cite journal |last=Bobylev |first=Vadim V. |authorlink= |date=March 2010 |title=Searching for Stars Closely Encountering with the Solar System |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |doi=10.1134/S1063773710030060 |arxiv=1003.2160 |bibcode=2010AstL...36..220B}}</ref> There is even a 1/10,000 chance of the star penetrating into the region (d < 1,000 AU) where the influence of the passing star on [[Kuiper belt]] objects is significant.<ref name="Bobylev:arXiv1003.2160"/>
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| The star with the second greatest perturbational effect in the past or future 10 million years was [[Algol]],<ref name="García-Sánchez1999">{{cite journal
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| | author=García-Sánchez, Joan
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| | title=Stellar Encounters with the Oort Cloud Based on HIPPARCOS Data
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| | journal=The Astronomical Journal | volume=117 | issue=2
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| | pages=1042–1055 |date=February 1999
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| | doi=10.1086/300723 | bibcode=1999AJ....117.1042G
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| | display-authors=1
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| | last2=Preston
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| | first2=Robert A.
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| | last3=Jones
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| | first3=Dayton L.
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| | last4=Weissman
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| | first4=Paul R.
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| | last5=Lestrade
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| | first5=Jean-François
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| | last6=Latham
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| | first6=David W.
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| | last7=Stefanik
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| | first7=Robert P. }}</ref> a triple star system that passed no closer than 9.8 light years, 7.3 million years ago, but with a considerably larger total mass of 5.8 solar masses.
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| == See also ==
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| * [[List of nearest stars]]
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| == Notes ==
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| {{reflist|group=note|refs=
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| {{#tag:ref|From apparent magnitude and parallax: <math>\scriptstyle M_V = m_V - 5 \log_{10} \left( \frac{100}{\mathrm{parallax\ in\ milliarcseconds}} \right)</math>|group="note"|name=absolute_magnitude}}
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| {{#tag:ref|Using the absolute visual magnitude of Gliese 710 <math>\scriptstyle M_{V_{\ast}}=8.23</math> and the absolute visual magnitude of the Sun <math>\scriptstyle M_{V_{\odot}}=4.83</math>, the visual luminosity can be calculated by <math>\scriptstyle \frac{L_{V_{\ast}}}{L_{V_{\odot}}}=10^{0.4\left(M_{V_{\odot}} - M_{V_{\ast}}\right)}</math>|group="note"|name=luminosity_visual}}
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| }}
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| ==References==
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| {{reflist|30em|refs=
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| <ref name=aaa474_2_653>{{cite journal | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | arxiv=0708.1752 }}</ref>
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| <ref name="Johnson">{{cite journal | last1=Johnson | first1=H. M. | last2=Wright | first2=C. D. | title=Predicted infrared brightness of stars within 25 parsecs of the sun | journal=The Astrophysical Journal Supplement Series | volume=53 | pages=643–711 |date=November 1983 | doi=10.1086/190905 | bibcode=1983ApJS...53..643J }}</ref>
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| <ref name=aj132_1_161>{{cite journal | display-authors=1 | last1=Gray | first1=R. O. | first2=C. J. | last2=Corbally | first3=R. F. | last3=Garrison | first4=M. T. | last4=McFadden | first5=P. E. | last5=Robinson | title=Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I | journal=The Astronomical Journal | volume=132 | issue=1 | pages=161–170 |date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G |arxiv = astro-ph/0603770 }}</ref>
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| <ref name=gcvs71>{{citation | display-authors=1 | last1=Kukarkin | first1=B. V. | last2=Kholopov | first2=P. N. | last3=Pskovsky | first3=Y. P. | last4=Efremov | first4=Y. N. | last5=Kukarkina | first5=N. P. | last6=Kurochkin | first6=N. E. | last7=Medvedeva | first7=G. I. | contribution=The third edition containing information on 20437 variable stars discovered and designated till 1968 | year=1971 | title=General Catalogue of Variable Stars | edition=3rd | bibcode=1971GCVS3.C......0K }}</ref>
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| <ref name=aaa514_A97>{{citation | display-authors=1 | last1=López-Santiago | first1=J. | last2=Montes | first2=D. | last3=Gálvez-Ortiz | first3=M. C. | last4=Crespo-Chacón | first4=I. | last5=Martínez-Arnáiz | first5=R. M. | last6=Fernández-Figueroa | first6=M. J. | last7=de Castro | first7=E. | last8=Cornide | first8=M. | title=A high-resolution spectroscopic survey of late-type stars: chromospheric activity, rotation, kinematics, and age | journal=Astronomy and Astrophysics | volume=514 | page=A97 |date=May 2010 | doi=10.1051/0004-6361/200913437 | bibcode=2010A&A...514A..97L |arxiv = 1002.1663 }}</ref>
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| <ref name="SIMBAD-Gliese710">{{cite web | title=Gliese 710 | work=SIMBAD Astronomical Database | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gliese+710 | accessdate=2010-03-18 }}</ref>
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| <ref name="bolometric_correction">{{citation | display-authors=1 | last1=Flower | first1=Phillip J.| title=Transformations from Theoretical Hertzsprung-Russell Diagrams to Color-Magnitude Diagrams: Effective Temperatures, B-V Colors, and Bolometric Corrections | url=http://articles.adsabs.harvard.edu//full/1996ApJ...469..355F/0000360.000.html | journal=[[The Astrophysical Journal]] | volume=469 | page=355 |date=September 1996 | doi=10.1086/177785| bibcode=1996ApJ...469..355F }}</ref>
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| <ref name="tableprovisoBC">{{cite journal | author=Torres, Guillermo | title=On the Use of Empirical Bolometric Corrections for Stars | url=http://iopscience.iop.org/1538-3881/140/5/1158/fulltext/ | journal=[[The Astronomical Journal]] |date=November 2010 | volume=140 | issue=5 | pages=1158–1162 | layurl=http://iopscience.iop.org/1538-3881/140/5/1158/fulltext/aj363350t3_ascii.txt | doi=10.1088/0004-6256/140/5/1158 | bibcode=2010AJ....140.1158T |arxiv = 1008.3913 }}</ref>
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| }}
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| ==Further reading==
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| *{{cite journal |last=García-Sánchez |first=Joan |authorlink= |year=1999 |month= |title=Stellar encounters with the Oort cloud based on ''Hipparcos'' data |journal=The Astronomical Journal |volume=117 |issue= 2|pages=1042–1055 |doi=10.1086/300723 |url= |accessdate= |quote= |bibcode=1999AJ....117.1042G |display-authors=1 |last2=Preston |first2=Robert A. |last3=Jones |first3=Dayton L. |last4=Weissman |first4=Paul R. |last5=Lestrade |first5=Jean-François |last6=Latham |first6=David W. |last7=Stefanik |first7=Robert P.}}
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| *{{cite journal
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| |last=García-Sánchez |first=J.
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| |coauthors=Weissman, P. R.; Preston, R. A.; Jones, D. L.; Lestrade, J.-F.; Latham, D. W.; Stefanik, R. P.; Paredes, J. M.
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| |title=Stellar encounters with the solar system
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| |journal=Astronomy and Astrophysics
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| |year=2001 |volume=379
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| |issue=2 |pages=634–659
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| |bibcode=2001A&A...379..634G
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| |doi=10.1051/0004-6361:20011330}}
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| *{{cite journal |last=Bobylev |first=Vadim V. |authorlink= |year=2010 |title=Searching for Stars Closely Encountering with the Solar System |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |doi=10.1134/S1063773710030060 |arxiv=1003.2160 |bibcode=2010AstL...36..220B}}
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| ==External links==
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| * [http://www.solstation.com/stars2/gl710.htm SolStation.com]
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| * [http://vizier.u-strasbg.fr/viz-bin/VizieR-S?NSV%2010635 VizieR variable star database]
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| * Wikisky [http://www.wikisky.org/?ra=18.33079&de=-1.9386054999999998&zoom=8&show_grid=1&show_constellation_lines=1&show_constellation_boundaries=1&show_const_names=0&show_galaxies=1&show_box=1&box_ra=18.33079&box_de=-1.9386055&box_width=50&box_height=50&img_source=DSS2 image] of HD 168442 (Gliese 710)
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| {{Nearest star systems|13}}
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| {{Stars of Serpens}}
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| [[Category:Durchmusterung objects|BD-01 03474]]
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| [[Category:Henry Draper Catalogue objects|168442]]
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| [[Category:Hipparcos objects|089825]]
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| [[Category:Gliese and GJ objects|0710]]
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| [[Category:K-type main-sequence stars]]
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| [[Category:Serpens (constellation)]]
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| [[Category:Objects within 100 ly of Earth]]
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