U Orionis
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 05h 55m 49.1689s |
| Declination | +20° 10′ 30.687″ |
| Apparent magnitude (V) | 4.8 - 13.0 |
| Characteristics | |
| Spectral type | M8III |
| B−V color index | 1.26 |
| Variable type | Mira-type |
| Astrometry | |
| Parallax (π) | 2.29 ± 1.21 mas |
| Distance | 997.56 ly (306±61 [1] pc) |
| Details | |
| Mass | ≥1.5 M☉ |
| Radius | 370±96[2] R☉ |
| Luminosity | 7000[3] L☉ |
| Temperature | ≈2750[3] K |
| Other designations | |
U Ori, HIP 28041, HD 39816,HR 2063, BD+20 1171a, RAFGL 837, SAO 77730 | |
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 from the United Kingdom for over 120 years. 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.[4]
Stellar parameters
The star has a low effective temperature (roughly 2700 K) but a large and bloated radius of 370 solar radii[2] and a high luminosity, 7,000 times higher than the Sun.[3] If the Sun were replaced with U Orionis, its radius would extend beyond Mars's orbital zone (about 1.7 astronomical units), and, to be habitable with water at liquid state and a comfortable temperature, a planet would have to be located within 85 AU, within the Kuiper belt's orbital zone.
Hints of a planetary system?
According to Rudnitskij,[5] 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
- ↑ Mondal (2005). "Evidence of asymmetry in Mira variable U Ori". Bulletin of the Astronomical Society of India. 33 (2): 97–102. Bibcode:2005BASI...33...97M.
- 1 2 Van Belle; et al. (1996). "Angular Size Measurements of 18 Mira Variable Stars at 2.2 microns". Astronomical Journal. 112: 2147. Bibcode:1996AJ....112.2147V. doi:10.1086/118170.
- 1 2 3 Mondal & Chandrasekhar (2004). "Evidence of asymmetry in Mira variable U Ori". Monthly Notices of the Royal Astronomical Society. 348 (4): 1332–1336. Bibcode:2004MNRAS.348.1332M. doi:10.1111/j.1365-2966.2004.07454.x.
- ↑ Monck (1887). "Mr Gore's Nova Orionis". The Observatory. 10: 69–71. Bibcode:1887Obs....10...69M.
- ↑ Rudnitskij (2002). "Molecular Masers in Variable Stars". Publications of the Astronomical Society of Australia. 19 (4): 499–504. Bibcode:2002PASA...19..499R. doi:10.1071/AS02018.