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Gliese 412

Coordinates: Sky map 11h 05m 22.3101s, +43° 31′ 51.0404″
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Gliese 412 A/B
Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Major
Gliese 412 A
Right ascension 11h 05m 22.3101s[1]
Declination +43° 31′ 51.0404″[1]
Apparent magnitude (V) 8.68[2]
Gliese 412 B
Right ascension 11h 05m 30.8856s[3]
Declination +43° 31′ 17.8843″[3]
Apparent magnitude (V) 14.45[4]
Characteristics
Spectral type M1.0V[2]/M6.0V[4]
U−B color index +1.16/—[5]
B−V color index +1.54[5]/2.08[6]
Astrometry
Gliese 412 A
Radial velocity (Rv)+64.9 ± 0.9[7] km/s
Proper motion (μ) RA: −4410.43±0.78[8] mas/yr
Dec.: 942.93±0.70[8] mas/yr
Parallax (π)203.8876 ± 0.0332 mas[9]
Distance15.997 ± 0.003 ly
(4.9047 ± 0.0008 pc)
Absolute magnitude (MV)10.34[10]
Gliese 412 B
Proper motion (μ) RA: −4339.891±0.167 mas/yr
Dec.: 960.780±0.162 mas/yr
Parallax (π)203.8323 ± 0.0500 mas[11]
Distance16.001 ± 0.004 ly
(4.906 ± 0.001 pc)
Absolute magnitude (MV)16.05[10]
Details
GJ 412 A
Mass0.48[10] M☉
Radius0.398±0.009[12] R☉
Surface gravity (log g)4.90[13] cgs
Temperature3,687[13]/ K
Metallicity [Fe/H]-0.43[13] dex
Rotational velocity (v sin i)<3[14] km/s
Age3[15] Gyr
GJ 412 B
Mass0.10[10] M☉
Radius0.13[15] R☉
Temperature2,700[6] K
Metallicity [Fe/H]−0.32[15] dex
Rotational velocity (v sin i)7.7±1.7[14] km/s
Other designations
BD+44°2051, GJ 412, CCDM J11055+4332AB, WDS J11055+4332AB[16][2]

A: Gaia DR2 778947814402405120, HIP 54211, SAO 43609, G 176-11, LAL 21258, LFT 757, LHS 38, LTT 12976, NLTT 26245[2]

B: WX UMa, Gaia DR2 778947608243864320, G 176-12, LFT 758, LHS 39, LTT 12977, NLTT 26247[4]
Database references
SIMBADThe system
A
B
Gliese 412 is located in the constellation Ursa Major.
Gliese 412 is located in the constellation Ursa Major.
Gliese 412
Location of Gliese 412 in the constellation Ursa Major

Gliese 412 is a pair of stars that share a common proper motion through space and are thought to form a binary star system. The pair have an angular separation of 31.4″ at a position angle of 126.1°.[17] They are located 15.8 light-years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.

The two stellar components of this system have a projected separation of about 152 AU, and an estimated orbital semimajor axis of 190 AU.[18] The primary has about 48% of the Sun's mass, while the secondary is only 10%.[10] The primary has a projected rotation velocity at the equator of less than 3 km/s; the secondary has a rotation velocity of 7.7±1.7 km/s.[14]

The primary star was monitored for radial velocity (RV) variations caused by a Jupiter-mass companion in a short-period orbit. It displayed no significant excess of RV variation that could be attributed to a planet.[19] A search of the system using near-infrared speckle interferometry also failed to detect a companion orbiting at distances of 1–10 AU.[20] Nor has a brown dwarf been detected orbiting within this system.[21]

The space velocity components of this system are U = 141, V = –7 and W = 7. They are members of the halo population of the Milky Way galaxy.[14]

X-ray source

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The secondary is a flare star that is referred to as WX Ursae Majoris. It is characterized as a UV Ceti-type variable star that displays infrequent increases in luminosity. This star was observed to flare as early as 1939 by the Dutch astronomer Adriaan van Maanen.[22]

Component B (WX Ursae Majoris) has been identified as an X-ray source, while no significant X-ray emission was detected from component A.[23] This system had not been studied in X-rays prior to ROSAT.[23] The Gaia DR2 release gives a parallax of 204.059 ±0.169 mas for B, indicating a distance of around 16 light-years.[3]

References

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  1. ^ a b 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.
  2. ^ a b c d "BD+44 2051". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  3. ^ a b c 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.
  4. ^ a b c "BD+44 2051B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  5. ^ a b Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Observatory. Bibcode:1978ppch.book.....N.
  6. ^ a b Casagrande, Luca; et al. (September 2008). "M dwarfs: effective temperatures, radii and metallicities". Monthly Notices of the Royal Astronomical Society. 389 (2): 585–607. arXiv:0806.2471. Bibcode:2008MNRAS.389..585C. doi:10.1111/j.1365-2966.2008.13573.x. S2CID 14353142.
  7. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. Bibcode:1967IAUS...30...57E.
  8. ^ a b van Leeuwen, F. (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.Vizier catalog entry
  9. ^ 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.
  10. ^ a b c d e "The 100 nearest star systems". Research Consortium On Nearby Stars. 2009-09-14. Archived from the original on 2007-11-12. Retrieved 2009-09-14.
  11. ^ 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.
  12. ^ Schweitzer, Andreas; Passegger, V. M.; Cifuentes, C.; Bejar, V. J. S.; Cortes-Contreras, M.; Caballero, J. A.; del Burgo, C.; Czesla, S.; Kuerster, M.; Montes, D.; Osorio, M. R. Zapatero; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J. (May 2019). "The CARMENES search for exoplanets around M dwarfs: Different roads to radii and masses of the target stars". Astronomy & Astrophysics. 625: A68. arXiv:1904.03231. doi:10.1051/0004-6361/201834965. ISSN 0004-6361.
  13. ^ a b c Soubiran, C.; Bienaymé, O.; Mishenina, T. V.; Kovtyukh, V. V. (March 2008). "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants". Astronomy and Astrophysics. 480 (1): 91–101. arXiv:0712.1370. Bibcode:2008A&A...480...91S. doi:10.1051/0004-6361:20078788. S2CID 16602121.
  14. ^ a b c d Delfosse, Xavier; Forveille, Thierry; Perrier, Christian; Mayor, Michel (March 1998). "Rotation and chromospheric activity in field M dwarfs". Astronomy and Astrophysics. 331: 581–595. Bibcode:1998A&A...331..581D.
  15. ^ a b c Mann, Andrew W.; et al. (May 2015), "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius", The Astrophysical Journal, 804 (1): 38, arXiv:1501.01635, Bibcode:2015ApJ...804...64M, doi:10.1088/0004-637X/804/1/64, S2CID 19269312, 64.
  16. ^ "** VBS 18". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-05-05.
  17. ^ Gould, Andrew; Chanamé, Julio (February 2004). "New Hipparcos-based Parallaxes for 424 Faint Stars". The Astrophysical Journal Supplement Series. 150 (2): 455–464. arXiv:astro-ph/0309001. Bibcode:2004ApJS..150..455G. doi:10.1086/381147. S2CID 8494577.
  18. ^ Reid, I. Neill; Gizis, John E. (June 1997). "Low-Mass Binaries and the Stellar Luminosity Function". Astronomical Journal. 113: 2246–2269. Bibcode:1997AJ....113.2246R. doi:10.1086/118436.
  19. ^ Endl, Michael; et al. (September 2006). "Exploring the Frequency of Close-in Jovian Planets around M Dwarfs". The Astrophysical Journal. 649 (1): 436–443. arXiv:astro-ph/0606121. Bibcode:2006ApJ...649..436E. doi:10.1086/506465. S2CID 14461746.
  20. ^ Leinert, C.; et al. (September 1997). "A search for companions to nearby southern M dwarfs with near-infrared speckle interferometry". Astronomy and Astrophysics. 325: 159–166. Bibcode:1997A&A...325..159L.
  21. ^ Oppenheimer, B. R.; et al. (April 2001). "A Coronagraphic Survey for Companions of Stars within 8 Parsecs". The Astronomical Journal. 121 (4): 2189–2211. arXiv:astro-ph/0101320. Bibcode:2001AJ....121.2189O. doi:10.1086/319941. S2CID 119092593.
  22. ^ Joy, Alfred H. (June 1967). "Stellar Flares". Astronomical Society of the Pacific Leaflets. 10 (456): 41–48. Bibcode:1967ASPL...10...41J.
  23. ^ a b Schmitt JHMM; Fleming TA; Giampapa MS (September 1995). "The X-Ray View of the Low-Mass Stars in the Solar Neighborhood". Astrophys. J. 450 (9): 392–400. Bibcode:1995ApJ...450..392S. doi:10.1086/176149.

See also

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