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Gliese 710

For the song, seeGliese 710 (song).

Gliese 710,orHIP 89825,is an orange 0.6M☉starin theconstellationSerpensCauda. It is projected to pass near theSunin about 1.29 million years at a predicted minimum distance of 0.051parsecs—0.1663light-years(10,520astronomical units)[5](about 1.6 trillion km)—about 1/25th of the current distance toProxima Centauri.[10]Such a distance would make for a similar brightness to the brightest planets, optimally reaching anapparent visual magnitudeof about −2.7. The star'sproper motionwill peak around onearcminuteper year,[11][12]a rate of apparent motion that would be noticeable over a human lifespan. This is a timeframe, based on data fromGaiaDR3,well within the parameters of current models which cover the next 15 million years.

Gliese 710
Observation data
EpochJ2000EquinoxJ2000
Constellation Serpens
Right ascension 18h19m50.8412s[1]
Declination −01° 56′ 19.005″[1]
Apparent magnitude(V) 9.66[2](9.65–9.69)[3]
Characteristics
Spectral type K7 Vk[4]
U−Bcolor index +1.26[2]
B−Vcolor index +1.37[2]
Variable type Suspected[3]
Astrometry
Radial velocity(Rv)−14.53±0.44[5]km/s
Proper motion(μ)RA:−0.414±0.019[5]mas/yr
Dec.:−0.108±0.017[5]mas/yr
Parallax(π)52.3963 ± 0.0171mas[5]
Distance62.25 ± 0.02ly
(19.085 ± 0.006pc)
Absolute magnitude(MV)8.20[6](8.19–8.23)[note 1]
Details
Mass0.57[7]M☉
Radius0.58[7]R☉
Luminosity (bolometric)0.091[7]L☉
Luminosity (visual, LV)0.045[note 2]L☉
Surface gravity(logg)4.66[7]cgs
Temperature4,143[7]K
Metallicity[Fe/H]−0.11[7]dex
Rotational velocity(vsini)6.42±0.78[8]km/s
Age300[9]Myr
Other designations
Gliese710,BD–01°3474,HIP89825,HD168442,NSV10635[2]
Database references
SIMBADdata
ARICNSdata

Description

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Gliese 710 currently is 62.3 light-years (19.1 parsecs) fromEarthin the constellationSerpensand has a below naked-eye visual magnitude of 9.69. Astellar classificationof K7 Vk means it is a smallmain-sequence starmostly generating energy through thethermonuclear fusionof hydrogen at its core. (The suffix 'k' indicates that the spectrum shows absorption lines from interstellar matter.) Stellar mass is about 57% of theSun's masswith an estimated 58% of theSun's radius.It is suspected to be avariable starthat may vary in magnitude from 9.65 to 9.69. As of 2020, no planets have been detectedorbitingit.

Computing and details of the closest approach

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An artist's rendering of theOort cloudand theKuiper belt(inset)

In their 2010 work, Bobylev et al. suggested that Gliese 710 has an 86% chance of passing through theOort cloud,assuming the Oort cloud to be a spheroid around the Sun with semiminor and semimajor axes of 80,000 and 100,000 AU, respectively. The distance of closest approach of Gliese 710 is generally difficult to compute precisely as it depends sensitively on its current position and velocity; Bobylev et al. estimated that Gliese 710 would pass within0.311±0.167 parsecs(1.014±0.545 light-years) of the Sun.[13]At the time, there was even a 1-in-10,000 chance of the star penetrating into the region (d < 1,000 AU) where the influence of the passing star onKuiper beltobjects would be significant.

Results from new calculations that include input data fromGaiaDR3indicate that the flyby of Gliese 710 to theSolar Systemwill on average be closer at0.051±0.003 pc(10,635±500 AU) in1.29±0.04 Matime, but with considerably less uncertainty.[5]The effects of such an encounter on the orbit of the Pluto–Charon system (and therefore, on the classical trans-Neptunian belt) are negligible, but Gliese 710 will traverse the outer Oort cloud (inside 100,000 AU or 0.48 pc) and reach the outskirts of the inner Oort cloud (inward of 20,000 AU).

Gliese 710 has the potential toperturbtheOort cloudin the outer Solar System, exerting enough force to send showers ofcometsinto the inner Solar System for millions of years, triggering visibility of about ten naked-eye comets per year,[12]and possibly causing animpact event.According to Filip Berski and Piotr Dybczyński, this event will be "the strongest disrupting encounter in the future and history of the Solar System."[14]Earlier dynamic models indicated that the net increase in cratering rate due to the passage of Gliese 710 would be no more than 5%.[15]They had originally estimated that the closest approach would happen in 1.36 million years when the star will approach within0.337±0.177 parsecs(1.100±0.577 light-years) of the Sun.[16]Gaia DR2 later found the minimumperiheliondistance to be0.0676±0.0157 parsecsor 13,900 ± 3,200 AU, about 1.281 million years from now.[17]

Table of parameters of predictions of Gliese 710 encounter with Sun

Source Date Encounter distance, pc Encounter time, Myr
[15] 1999 0.34 ± 0.18 pc (1.11 ± 0.59 ly) 1.36±0.04
[13] March 2010 0.311 ± 0.167 pc (1.01 ± 0.54 ly) 1.45±0.06
[11] November 2016 0.0648 ± 0.0303 pc (13,400 ± 6,200 AU) 1.35
[10] May 2018 0.052 ± 0.01 pc (10,700 ± 2,100 AU) 1.28±0.05
[17] May 2018 0.0676 ± 0.0157 pc (13,900 ± 3,200 AU) 1.281
[5] December 2020 0.051 ± 0.003 pc (10,520 ± 620 AU) 1.29±0.04
[18] June 2022 0.052 ± 0.002 pc (10,730 ± 410 AU) 1.29±0.02
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See also

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Notes

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  1. ^From apparent magnitude and parallax:
  2. ^Using the absolute visual magnitude of Gliese 710and the absolute visual magnitude of the Sun,the visual luminosity can be calculated by

References

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  1. ^abBrown, A. G. A.;et al. (Gaia collaboration) (August 2018)."GaiaData 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.Gaia DR2 record for this sourceatVizieR.
  2. ^abcd"GJ 710".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2019-07-06.
  3. ^abKukarkin, B. V.; et al. (1971). "The third edition containing information on 20437 variable stars discovered and designated till 1968".General Catalogue of Variable Stars(3rd ed.).Bibcode:1971GCVS3.C......0K.
  4. ^Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I".The Astronomical Journal.132(1): 161–170.arXiv:astro-ph/0603770.Bibcode:2006AJ....132..161G.doi:10.1086/504637.S2CID119476992.
  5. ^abcdefgde la Fuente Marcos, Raúl and de la Fuente Marcos, Carlos (2020)."An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia EDR3: Slightly Closer and a Tad Later than Previous Estimates".Research Notes of the AAS.4(12): 222.Bibcode:2020RNAAS...4..222D.doi:10.3847/2515-5172/abd18d.
  6. ^Koen, C.; Kilkenny, D.; Van Wyk, F.; Marang, F. (2010)."UBV(RI)C JHK observations of Hipparcos-selected nearby stars".Monthly Notices of the Royal Astronomical Society.403(4): 1949.Bibcode:2010MNRAS.403.1949K.doi:10.1111/j.1365-2966.2009.16182.x.
  7. ^abcdefSchweitzer, Andreas; et al. (May 2019). "The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars".Astronomy & Astrophysics.625:16.arXiv:1904.03231.Bibcode:2019A&A...625A..68S.doi:10.1051/0004-6361/201834965.S2CID102351979.A68.
  8. ^López-Santiago, J.; et al. (May 2010). "A high-resolution spectroscopic survey of late-type stars: chromospheric activity, rotation, kinematics, and age".Astronomy and Astrophysics.514:A97.arXiv:1002.1663.Bibcode:2010A&A...514A..97L.doi:10.1051/0004-6361/200913437.S2CID118640516.
  9. ^Passegger, V. M.; Schweitzer, A.; Shulyak, D.; Nagel, E.; Hauschildt, P. H.; Reiners, A.; Amado, P. J.; Caballero, J. A.; Cortés-Contreras, M.; Domínguez-Fernández, A. J.; Quirrenbach, A.; Ribas, I.; Azzaro, M.; Anglada-Escudé, G.; Bauer, F. F.; Béjar, V. J. S.; Dreizler, S.; Guenther, E. W.; Henning, T.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Martín, E. L.; Montes, D.; Morales, J. C.; Schmitt, J. H. M. M.; Zechmeister, M. (2019). "The CARMENES search for exoplanets around M dwarfs. Photospheric parameters of target stars from high-resolution spectroscopy. II. Simultaneous multiwavelength range modeling of activity insensitive lines".Astronomy and Astrophysics.627:627.arXiv:1907.00807.Bibcode:2019A&A...627A.161P.doi:10.1051/0004-6361/201935679.
  10. ^abde la Fuente Marcos, Raúl and de la Fuente Marcos, Carlos (2018)."An Independent Confirmation of the Future Flyby of Gliese 710 to the Solar System UsingGaia".Research Notes of the AAS.2(2): 30.arXiv:1805.02644.Bibcode:2018RNAAS...2...30D.doi:10.3847/2515-5172/aac2d0.S2CID119467738.
  11. ^abBerski, Filip and Dybczyński, Piotr A. (2016-11-01)."Gliese 710 will pass the Sun even closer".Astronomy & Astrophysics.595:L10.Bibcode:2016A&A...595L..10B.doi:10.1051/0004-6361/201629835.ISSN0004-6361.
  12. ^abDorminey, Bruce."Solar System's Next Close Encounter Will Be With Gliese 710, Say Astronomers".Forbes.Archivedfrom the original on 2016-12-24.Retrieved2016-12-24.
  13. ^abBobylev, Vadim V. (March 2010). "Searching for Stars Closely Encountering with the Solar System".Astronomy Letters.36(3): 220–226.arXiv:1003.2160.Bibcode:2010AstL...36..220B.doi:10.1134/S1063773710030060.S2CID118374161.
  14. ^Dvorsky, George."Incoming Star Could Spawn Swarms of Comets When It Passes Our Sun".Gizmodo.Archivedfrom the original on 2020-08-13.Retrieved2016-12-24.
  15. ^abGarcía-Sánchez, Joan; et al. (1999)."Stellar encounters with the Oort cloud based onHipparcosdata ".The Astronomical Journal.117(2): 1042–1055.Bibcode:1999AJ....117.1042G.doi:10.1086/300723.S2CID122929693.
  16. ^García-Sánchez, J.; Weissman, P. R.; Preston, R. A.; Jones, D. L.; Lestrade, J.-F.; Latham, D. W.; Stefanik, R. P.; Paredes, J. M. (2001)."Stellar encounters with the solar system".Astronomy and Astrophysics.379(2): 634–659.Bibcode:2001A&A...379..634G.doi:10.1051/0004-6361:20011330.
  17. ^abBailer-Jones, C.A.L.; Rybizki, J.; Andrae, R.; Fouesnea, M. (2018). "New stellar encounters discovered in the second Gaia data release".Astronomy & Astrophysics.616:A37.arXiv:1805.07581.Bibcode:2018A&A...616A..37B.doi:10.1051/0004-6361/201833456.S2CID56269929.
  18. ^de la Fuente Marcos, Raúl and de la Fuente Marcos, Carlos (2022)."An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia DR3: Flyby Parameters Reproduced, Uncertainties Reduced".Research Notes of the AAS.6(6): 136.Bibcode:2022RNAAS...6..136D.doi:10.3847/2515-5172/ac7b95.
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