U Orionis
Location of U Orionis (circled) | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 05h 55m 49.17076s[1] |
| Declination | +20° 10′ 30.6779″[1] |
| Apparent magnitude (V) | 4.8 - 13.0[2] |
| Characteristics | |
| Spectral type | M6e-M9.5e[2] |
| B−V color index | +2.07[3] |
| Variable type | Mira[2] |
| Astrometry | |
| Parallax (π) | 3.4924±0.1820 mas[1] |
| Distance | 930 ± 50 ly (290 ± 10 pc) |
| Details | |
| Mass | 0.88[4] M☉ |
| Radius | 370±96[5] R☉ |
| Luminosity | 7,000[6] L☉ |
| Surface gravity (log g) | −0.44[4] cgs |
| Temperature | 2,641[4] K |
| Metallicity [Fe/H] | 0.54[4] dex |
| Other designations | |
| U Ori, BD+20°1171a, HD 39816, HIP 28041, HR 2063, SAO 77730[7] | |
| Database references | |
| SIMBAD | data |
U Orionis (abbreviated U Ori) is a Mira-type variable star in the constellation Orion. It is a classical long period variable star that has been well observed for over 120 years.
Discovery
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It was discovered on 1885 December 13 by J.E. Gore and initially it was thought to be a nova in the early stages of decline (Gore's Nova and NOVA Ori 1885 as still listed in SIMBAD), but a spectrum taken at Harvard showed features similar to that of Mira. Thus U Orionis became the first long period variable to be identified by a photograph of its spectrum.[8]
Location
[edit | edit source]U Orionis lies less than half a degree east of the small-amplitude variable star χ1 Orionis and less than an arc-minute from the much fainter eclipsing variable UW Orionis. χ1 Orionis is slightly brighter than U Orionis at its brightest maximum, while UW Orionis is more than a thousand times fainter, similar to U Orionis at minimum.
Stellar parameters
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The star has a low effective temperature (variable with the pulsations, but roughly 2,700 K), a large and bloated radius of 370 R☉,[5] and a high luminosity, 7,000 times higher than the Sun.[6] If the Sun were replaced with U Orionis, its radius would extend beyond Mars's orbital zone (about 1.7 astronomical units).
Possible planetary system
[edit | edit source]According to Rudnitskij,[10] a 12- to 15-year "super-periodicity" has been observed. The author infers such periodicity could coincide with the revolution period of an invisible companion, probably planetary. So far no clear hint of planetary objects has been detected.
References
[edit | edit source]- ^ a b c Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value). (Erratum: Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).). Gaia EDR3 record for this source at VizieR.
- ^ a b c Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ a b c d Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ a b Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ a b Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
- ^ Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value).
