Gliese 412

Coordinates: Sky map 11h 05m 22.3101s, +43° 31′ 51.0404″
Source: Wikipedia, the free encyclopedia.
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]
Distance
16.001 ± 0.004 ly
(4.906 ± 0.001 pc)
Absolute magnitude (MV)16.05[10]
Details
GJ 412 A
Rotational velocity (v sin i)
7.7±1.7[14] km/s
BD+44°2051, GJ 412, CCDM J11055+4332AB, WDS J11055+4332AB[16][2]

A:

NLTT 26245[2]

B:
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

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.

This system, also known as Lalande 21258, was announced in 1860 as a high apparent proper motion star by

Bonner Durchmusterung (BD).[18] 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.[19]

The two stellar components of this system have a

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.[21] A search of the system using near-infrared speckle interferometry also failed to detect a companion orbiting at distances of 1–10 AU.[22] Nor has a brown dwarf been detected orbiting within this system.[23]

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

The secondary is 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.[24]

Component B (WX Ursae Majoris) has been identified as an X-ray source, while no significant X-ray emission was detected from component A.[25] This system had not been studied in X-rays prior to ROSAT.[25] 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

  1. ^
    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. ^
    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. ^
    Bibcode:1978ppch.book.....N
    .
  6. ^
    S2CID 14353142
    .
  7. Bibcode:1967IAUS...30...57E
    .
  8. ^
    doi:10.1051/0004-6361:20078357.Vizier catalog entry
  9. 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. doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR
    .
  12. ISSN 0004-6361
    .
  13. ^
    S2CID 16602121
    .
  14. ^
    Bibcode:1998A&A...331..581D
    .
  15. ^
    S2CID 19269312
    , 64.
  16. ^ "** VBS 18". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-05-05.
  17. S2CID 8494577
    .
  18. ^ F.W.A. Argelander (December 1860). "Mittheilungen von Herrn Professor Argelander". Astronomische Nachrichten. 54: 243–244.
  19. ^ Adalbert Krueger (February 1863). "Ueber die Parallaxe des Sterns LL. 21258". Acta Societatis Scientiarum Fennicae. 7: 375–376.
  20. doi:10.1086/118436
    .
  21. S2CID 14461746
    .
  22. Bibcode:1997A&A...325..159L
    .
  23. S2CID 119092593
    .
  24. Bibcode:1967ASPL...10...41J
    .
  25. ^
    doi:10.1086/176149
    .

See also
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