Gliese 412

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°.[14] They are located 15.8 light years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.

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)206.27 ± 1.00[8] mas
Distance15.81 ± 0.08 ly
(4.85 ± 0.02 pc)
Absolute magnitude (MV)10.34[9]
Gliese 412 B
Proper motion (μ) RA: −4339.891±0.167 mas/yr
Dec.: 960.780±0.162 mas/yr
Parallax (π)204.0592 ± 0.1687[3] mas
Distance15.98 ± 0.01 ly
(4.901 ± 0.004 pc)
Absolute magnitude (MV)16.05[9]
Details
GJ 412 A
Mass0.48[9] M☉
Radius0.38[10] R☉
Surface gravity (log g)4.90[11] cgs
Temperature3,687[11]/ K
Metallicity [Fe/H]-0.43[11] dex
Rotational velocity (v sin i)<3[12] km/s
Age3[10] Gyr
GJ 412 B
Mass0.10[9] M☉
Radius0.13[10] R☉
Temperature2,700[6] K
Metallicity [Fe/H]−0.32[10] 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[13][2]

A: Gaia DR2 778947814402405120, HIP 54211, SAO 43609, G 176-11, 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

The two stellar components of this system have a projected separation of about 152 AU, and an estimated orbital semimajor axis of 190 AU.[15] The primary has about 48% of the Sun's mass, while the secondary is only 10%.[9] 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.[12]

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.[16] A search of the system using near-infrared speckle interferometry also failed to detect a companion orbiting at distances of 1–10 AU.[17] Nor has a brown dwarf been detected orbiting within this system.[18]

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.[19]

Component B (WX Ursae Majoris) has been identified as an X-ray source, while no significant X-ray emission was detected from component A.[20] This system had not been studied in X-rays prior to ROSAT.[20] The Gaia DR2 release gives a parallax of 204.059±0.169 mas for B, indicating a distance of around 16 ly.[3]

gollark: Huh, this is neat, apparently nginx is scriptable with Lua.
gollark: This is a clear sign of the impending apocalypse.
gollark: All hail ffmpeg.
gollark: Hey, don't ðelete your messages after someone cricitizes you.
gollark: What's wrong with Wojbie? He's cool!

References
  1. 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. "BD+44 2051". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  3. 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. "BD+44 2051B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  5. Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Observatory. Bibcode:1978ppch.book.....N.
  6. 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.
  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. 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. "The 100 nearest star systems". Research Consortium On Nearby Stars. 2009-09-14. Retrieved 2009-09-14.
  10. 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, 64.
  11. 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.
  12. Delfosse, X.; et al. (March 1998). "Rotation and chromospheric activity in field M dwarfs". Astronomy and Astrophysics. 331: 581–595. Bibcode:1998A&A...331..581D.
  13. "VBS 18". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  14. 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.
  15. 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.
  16. 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.
  17. 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.
  18. 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.
  19. Joy, Alfred H. (June 1967). "Stellar Flares". Astronomical Society of the Pacific Leaflets. 10 (456): 41–48. Bibcode:1967ASPL...10...41J.
  20. 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
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.