Gliese 412
Gliese 412 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
Observation dataEpoch J2000      Equinox J2000
ConstellationUrsa Major[1][2]
Gliese 412 A
Right ascension11h 05m 28.57695s[3]
Declination+43° 31′ 36.3869″[3]
Apparent magnitude (V)8.68[4]
Gliese 412 B
Right ascension11h 05m 30.88558s[5]
Declination+43° 31′ 17.8852″[5]
Apparent magnitude (V)14.45[6]
Characteristics
Gliese 412 A
Spectral typeM1.0V[4]
U−B color index+1.16[7]
B−V color index+1.54[7]
Gliese 412 B
Spectral typeM6.0V[6]
B−V color index+2.08[8]
Astrometry
Gliese 412 A
Radial velocity (Rv)+68.41±0.12[3] km/s
Proper motion (μ)RA: −4,406.469mas/yr[3]Dec.: +938.527mas/yr[3]
Parallax (π)203.8876±0.0332 mas[3]
Distance15.997 ± 0.003 ly (4.9047 ± 0.0008 pc)
Absolute magnitude (MV)10.34[9]
Gliese 412 B
Radial velocity (Rv)+67.94±0.74[5] km/s
Proper motion (μ)RA: −4,339.850mas/yr[5]Dec.: +960.696mas/yr[5]
Parallax (π)203.8323±0.0500 mas[5]
Distance16.001 ± 0.004 ly (4.906 ± 0.001 pc)
Absolute magnitude (MV)16.05[9]
Details
Gliese 412 A
Mass0.387±0.010[10] M☉
Radius0.398±0.009[10] R☉
Luminosity0.0223±0.0004[10] L☉
Surface gravity (log g)4.860±0.031[10] cgs
Temperature3,639±51[10] K
Metallicity[Fe/H]−0.30±0.16[10] dex
Rotation36.9±2.5 d[11]
Rotational velocity (v sin i)<3[12] km/s
Age3[13] Gyr
Gliese 412 B
Mass0.0952±0.0095[13] M☉
Radius0.1262±0.0054[13] R☉
Luminosity0.000915±0.000024[14] L☉
Temperature2,863±60[13] K
Metallicity[Fe/H]−0.32±0.08[13] dex
Rotational velocity (v sin i)7.7±1.7[12] km/s
Other designations
BD+44°2051, GJ 412, CCDM J11055+4332AB, WDS J11055+4332AB[15][4]

A:Gaia DR2 778947814402405120, HIP 54211, SAO 43609, G 176-11, LAL 21258, LFT 757, LHS 38, LTT 12976, NLTT 26245[4]

B:WX UMa, Gaia DR2 778947608243864320, G 176-12, LFT 758, LHS 39, LTT 12977, NLTT 26247[6]
Database references
SIMBADA
B

Gliese 412 is a binary star system in the constellation Ursa Major. Among the nearest stars, they lie at a distance of 16.0 light-years (4.9 parsecs). The pair have an angular separation of 31.4″ at a position angle of 126.1°.[16] Both components are relatively dim red dwarf stars.

History of observations

This system, also known as Lalande 21258, was announced in 1860 as a high apparent proper motion star by Friedrich Wilhelm Argelander as a result of work on the Bonner Durchmusterung (BD).[17]Adalbert Krueger, an assistant to the BD project, was tasked with measuring its parallax. In Krueger's paper reporting the result, he dubbed it Argelander's Third Star.[18]

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]

Characteristics

The two stellar components of this system have a projected separation of about 152 AU, and an estimated orbital semimajor axis of 190 AU.[22]

The primary has 0.387 times the mass of the Sun, 0.398 times the Sun's radius and 2.23% of the Sun's luminosity.[10] It is spinning at a rotation velocity at the equator of less than 3 km/s.[12] The secondary is smaller and fainter, at 9.52% of the Sun's mass, 12.62% of the Sun's radius[13] and luminosity only 0.09% solar.[14] It is spinning at a rotation velocity of 7.7±1.7 km/s.[12] Gliese 412 A has a temperature of 3,639 K,[10] while Gliese 412 B has 2,863 K.[13]

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.[12]

X-ray source

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.[23]

Component B (WX Ursae Majoris) has been identified as an X-ray source, while no significant X-ray emission was detected from component A.[24] This system had not been studied in X-rays prior to ROSAT.[24]

References

  1. ^Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034.Constellation record for this object at VizieR.
  2. ^Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034.Constellation record for this object at VizieR.
  3. ^ abcdeVallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875.Gaia DR3 record for this source at VizieR.
  4. ^ abcd"BD+44 2051". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  5. ^ abcdeVallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875.Gaia DR3 record for this source at VizieR.
  6. ^ abc"BD+44 2051B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  7. ^ abNicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Observatory. Bibcode:1978ppch.book.....N.
  8. ^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.
  9. ^ ab"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.
  10. ^ abcdefghSchweitzer, 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. Bibcode:2019A&A...625A..68S. doi:10.1051/0004-6361/201834965. ISSN 0004-6361.
  11. ^Donati, J.-F.; Lehmann, L. T.; et al. (October 2023). "Magnetic fields and rotation periods of M dwarfs from SPIRou spectra". Monthly Notices of the Royal Astronomical Society. 525 (2): 2015–2039. arXiv:2307.14190. Bibcode:2023MNRAS.525.2015D. doi:10.1093/mnras/stad2301.
  12. ^ abcdeDelfosse, 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.
  13. ^ abcdefgMann, 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.
  14. ^ abHardegree-Ullman, Kevin K.; Apai, Dániel; Bergsten, Galen J.; Pascucci, Ilaria; López-Morales, Mercedes (2023). "Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O2 Levels in Nearby Transiting Habitable-zone Exoplanets". The Astronomical Journal. 165 (6): 267. arXiv:2304.12490. Bibcode:2023AJ....165..267H. doi:10.3847/1538-3881/acd1ec.
  15. ^"** VBS 18". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-05-05.
  16. ^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.
  17. ^F.W.A. Argelander (December 1860). "Mittheilungen von Herrn Professor Argelander". Astronomische Nachrichten. 54: 243–244.
  18. ^Adalbert Krueger (February 1863). "Ueber die Parallaxe des Sterns LL. 21258". Acta Societatis Scientiarum Fennicae. 7: 375–376.
  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. ^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.
  23. ^Joy, Alfred H. (June 1967). "Stellar Flares". Astronomical Society of the Pacific Leaflets. 10 (456): 41–48. Bibcode:1967ASPL...10...41J.
  24. ^ abSchmitt 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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