Gliese 412

Gliese 412 A/B
Gliese 412
Location of Gliese 412 in the constellation Ursa Major

Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Major[1][2]
Gliese 412 A
Right ascension 11h 05m 28.57695s[3]
Declination +43° 31′ 36.3869″[3]
Apparent magnitude (V) 8.68[4]
Gliese 412 B
Right ascension 11h 05m 30.88558s[5]
Declination +43° 31′ 17.8852″[5]
Apparent magnitude (V) 14.45[6]
Characteristics
Gliese 412 A
Spectral type M1.0V[4]
U−B color index +1.16[7]
B−V color index +1.54[7]
Gliese 412 B
Spectral type M6.0V[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: −4,406.469 mas/yr[3]
Dec.: +938.527 mas/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: −4,339.850 mas/yr[5]
Dec.: +960.696 mas/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
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. ^ a b c d e Vallenari, 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. ^ a b c d "BD+44 2051". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  5. ^ a b c d e Vallenari, 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. ^ a b c "BD+44 2051B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  7. ^ a b Nicolet, 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. ^ a b "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. ^ a b c d e f g h 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. 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. ^ a b c d e 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.
  13. ^ a b c d e f g 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.
  14. ^ a b Hardegree-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. ^ 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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