Gliese 710

Gliese 710, or HIP 89825, is an orange 0.6 M☉ star in the constellation Serpens Cauda. It is projected to pass near the Sun in a timeframe well within the parameters of current models which cover the next 15 million years. The predicted minimum distance will occur in about 1.281 million years, with Gaia DR2 suggesting a slightly closer distance to the previous estimates of 0.0676 parsecs—0.221 light-years (14,000 astronomical units)[11]—a distance about 20 times closer than the current distance of Proxima Centauri. Such a distance would make for a similar brightness to the brightest planets, optimally reaching an apparent visual magnitude of about −2.7 (brighter than Mars at opposition). The star's proper motion will peak around one arcminute per year,[12][13] a rate of apparent motion that would be noticeable over a human lifespan.

Gliese 710
Observation data
Epoch J2000      Equinox J2000
Constellation Serpens
Right ascension  18h 19m 50.8412s[1]
Declination –01° 56′ 19.003″[1]
Apparent magnitude (V) 9.66[2] (9.65–9.69)[3]
Characteristics
Spectral type K7 Vk[4]
U−B color index +1.26[2]
B−V color index +1.37[2]
Variable type Suspected[3]
Astrometry
Radial velocity (Rv) –14.525 ± 0.435 km/s
Proper motion (μ) RA: -0.460 ± 0.084[5] mas/yr
Dec.: -0.028 ± 0.074[5] mas/yr
Parallax (π)52.519 ± 0.048[6] mas
Distance62.10 ± 0.06 ly
(19.04 ± 0.02 pc)
Absolute magnitude (MV)8.20[7] (8.19-8.23)[note 1]
Details
Mass0.6[8] M☉
Radius0.67[9] R☉
Luminosity (bolometric)0.100+0
−0.001[6] L☉
Luminosity (visual, LV)0.045[note 2] L☉
Temperature4,250[8] K
Rotational velocity (v sin i)6.42 ± 0.78[10] km/s
Other designations
Gliese 710, BD–01° 3474, HIP 89825, HD 168442, NSV 10635[2]
Database references
SIMBADdata
ARICNSdata

Description

Gliese 710 currently is 63.8 light-years (19.6 parsecs) from Earth in the constellation Serpens and has a below naked-eye visual magnitude of 9.69. A stellar classification of K7 Vk[4] means it is a small main-sequence star mostly generating energy through the thermonuclear fusion of hydrogen at its core. (The suffix 'k' indicates that the spectrum shows absorption lines from interstellar matter.) Stellar mass is about 60%[8] of the Sun's mass with an estimated 67% of the Sun's radius.[9] It is suspected to be a variable star that may vary in magnitude from 9.65 to 9.69. As of 2020, no planets have been detected orbiting it.

Computing and details of the closest approach
An artist's rendering of the Oort cloud and the Kuiper belt (inset)

Gliese 710 has the potential to perturb the Oort cloud in the outer Solar System, exerting enough force to send showers of comets into the inner Solar System for millions of years, triggering visibility of about ten naked-eye comets per year,[13] and possibly causing an impact 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%.[8] They had originally estimated that the closest approach would happen in 1,360,000 years when the star will approach within 0.337 ± 0.177 parsecs (1.100 ± 0.577 light-years) of the Sun.[15] Gaia DR2 now finds the minimum perihelion distance is 0.0676 ± 0.0157 parsecs or 13,900 ± 3,200 AU about 1.281 million years from now.[11]

Bobylev in 2010 further suggested Gliese 710 has an 86% chance of passing through the Oort cloud, assuming the Oort cloud to be a spheroid around the Sun with semiminor and semimajor axes of 80,000 and 100,000 AU. The distance of closest approach of Gliese 710 is difficult to compute precisely as it depends sensitively on its current position and velocity; Bobylev estimated that it would pass within 0.311 ± 0.167 parsecs (1.014 ± 0.545 light-years) of the Sun.[16] There is 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 on Kuiper belt objects is significant.

Table of parameters of predictions of Gliese 710 encounter with Sun

SourceDateEncounter distance, pcEncounter time, Myr
[8]19990.34 ± 0.18 pc (1.11 ± 0.59 ly)1.36 ± 0.04
[16]March 20100.311 ± 0.167 pc (1.01 ± 0.54 ly)1.45 ± 0.06
[17]May 20180.052 ± 0.01 pc (0.170 ± 0.033 ly)1.28 ± 0.05
[11]May 20180.0676 ± 0.0157 pc (0.220 ± 0.051 ly)1.281
gollark: "Sadness" is some complex state or collection of states or something which the brain gets in, generally because of a bad thing of some sort.
gollark: Or in my case complex "solid state farming" machines which grow trees in magic boxes.
gollark: REAL minecrafters set up industrial-scale deforestation machinery.
gollark: > emotions tell us as much about our environment and circumstance as touch or smell or sightThey really seem more like convenient brain heuristics than some sort of actual sensory input.
gollark: It's "free" because there's no money, but not actually-free as in it can be produced infinitely with no inputs.

See also

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

References
  1. Gaia Collaboration; Brown, A. G. A.; Vallenari, A.; Prusti, T.; De Bruijne, J. H. J.; Mignard, F.; Drimmel, R.; Babusiaux, C.; Bailer-Jones, C. A. L.; Bastian, U.; Biermann, M.; Evans, D. W.; Eyer, L.; Jansen, F.; Jordi, C.; Katz, D.; Klioner, S. A.; Lammers, U.; Lindegren, L.; Luri, X.; O'Mullane, W.; Panem, C.; Pourbaix, D.; Randich, S.; Sartoretti, P.; Siddiqui, H. I.; Soubiran, C.; Valette, V.; Van Leeuwen, F.; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics. 595: A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512.
  2. "GJ 710". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-06.
  3. Kukarkin, B. V.; et al. (1971). "The third edition containing information on 20437 variable stars discovered and designated till 1968". General Catalogue of Variable Stars. 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.
  5. van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  6. 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. Gaia DR2 record for this source at VizieR.
  7. 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.
  8. García-Sánchez, J.; et al. (1999). "Stellar encounters with the Oort cloud based on Hipparcos data". The Astronomical Journal. 117 (2): 1042–1055. Bibcode:1999AJ....117.1042G. doi:10.1086/300723.
  9. Johnson, H. M.; Wright, C. D. (November 1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". The Astrophysical Journal Supplement Series. 53: 643–711. Bibcode:1983ApJS...53..643J. doi:10.1086/190905.
  10. 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.
  11. Bailer-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.
  12. Berski, Filip; 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. ISSN 0004-6361.
  13. Dorminey, Bruce. "Solar System's Next Close Encounter Will Be With Gliese 710, Say Astronomers". Forbes. Retrieved 2016-12-24.
  14. Dvorsky, George. "Incoming Star Could Spawn Swarms of Comets When It Passes Our Sun". Gizmodo. Retrieved 2016-12-24.
  15. 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.
  16. Bobylev, 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.
  17. de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (10 May 2018). "An Independent Confirmation of the Future Flyby of Gliese 710 to the Solar System Using Gaia". Research Notes of the AAS. 2 (2): 30. arXiv:1805.02644. Bibcode:2018RNAAS...2b..30D. doi:10.3847/2515-5172/aac2d0.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.