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Possible binary star system in the constellation Ursa Major From Wikipedia, the free encyclopedia
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.
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] |
Distance | 15.997 ± 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] |
Distance | 16.001 ± 0.004 ly (4.906 ± 0.001 pc) |
Absolute magnitude (MV) | 16.05[10] |
Details | |
GJ 412 A | |
Mass | 0.48[10] M☉ |
Radius | 0.398±0.009[12] R☉ |
Surface gravity (log g) | 4.90[13] cgs |
Temperature | 3,687[13]/ K |
Metallicity [Fe/H] | -0.43[13] dex |
Rotational velocity (v sin i) | <3[14] km/s |
Age | 3[15] Gyr |
GJ 412 B | |
Mass | 0.10[10] M☉ |
Radius | 0.13[15] R☉ |
Temperature | 2,700[6] K |
Metallicity [Fe/H] | −0.32[15] dex |
Rotational velocity (v sin i) | 7.7±1.7[14] km/s |
Other designations | |
Database references | |
SIMBAD | The system |
A | |
B | |
Location of Gliese 412 in the constellation Ursa Major |
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]
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]
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