Chi(1) Orionis
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| Chi(1) Orionis A | |
| Stellar characteristics | |
|---|---|
| Constellation | Orion |
| Right ascension (Epoch J2000) | 05h 54m 22.98s |
| Declination (Epoch J2000) | +20° 16' 34.23" |
| Spectral type | G0 Ve |
| Distance from Sol | 28.3 ly |
| Other designations | Chi1 Ori, 54 Ori, HR 2047, Gl 222 A, Hip 27913, HD 39587, BD+20 1162, SAO 77705, LTT 11743. |
| Chi(1) Orionis B | |
| Stellar characteristics | |
|---|---|
| Constellation | Orion |
| Right ascension (Epoch J2000) | 05h 54m 22.98s |
| Declination (Epoch J2000) | +20° 16' 34.23" |
| Spectral type | M V? |
| Distance from Sol | 28.3 ly |
Chi(1) Orionis is a binary star system, located almost 28.3 light-years away from our Sun, Sol. It lies in the northeastern corner of the constellation Orion, the Hunter. The binary nature of the star system was discovered by Sarah Lee Lippincott and Michael D. Worth in 1978 based on astrometric analysis of photographic plates from 1937 to 1977[1]. The system is a member of the Ursa Major stellar moving group.
Spectroscopic, astrometric and radial-velocity analyses reveal a companion with an average separation of 6.4 AUs, varying between 3.5 and 9.3 AUs. The two stars move in an elliptical (e= 0.45) orbit that takes about 14.2 years to complete and is inclined at about 93° from the perspective of an observer on Earth[2][3].
Chi(1) Orionis A
Chi(1) Orionis is a yellow-orange main sequence dwarf star of spectral and luminosity type G0 V, with roughly the same mass as Sol[3], as much as 1.45 times its diameter[4], and less than 1.1 times its luminosity. It may be 89 to 178 percent as enriched as Sol with iron[5].
Chi(1) Orionis B
Analysis of radial velocity variations suggest that this probable red dwarf star has about 15 percent of Sol's mass [3].
(Data from SolStation.com)
Notes
- ↑ (Lippincott and Worth, 1978)
- ↑ (George G. Gatewood, 1994)
- ↑ 3.0 3.1 3.2 (Irwin et al, 1992)
- ↑ (George G. Gatewood, 1994, page 143)
- ↑ (Cayrel de Strobel et al, 1991, page 12)
