Astronomy:Omicron Coronae Borealis
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Corona Borealis |
| Right ascension | 15h 20m 08.559s[1] |
| Declination | +29° 36′ 58.35″[1] |
| Apparent magnitude (V) | +5.53[2] |
| Characteristics | |
| Spectral type | K0 III[3] |
| U−B color index | +0.786[2] |
| B−V color index | +1.009[2] |
| Astrometry | |
| Radial velocity (Rv) | −54.15±0.20[4] km/s |
| Proper motion (μ) | RA: −117.98±0.18[1] mas/yr Dec.: −42.44±0.31[1] mas/yr |
| Parallax (π) | 12.08 ± 0.44[1] mas |
| Distance | 270 ± 10 ly (83 ± 3 pc) |
| Absolute magnitude (MV) | +0.92[3] |
| Details[4] | |
| Mass | 1.07±0.19 M☉ |
| Radius | 10.13±0.40 R☉ |
| Luminosity | 50.1 L☉ |
| Surface gravity (log g) | 2.70±0.06 cgs |
| Temperature | 4,812±13 K |
| Metallicity [Fe/H] | −0.24±0.01 dex |
| Rotational velocity (v sin i) | 0.47±0.61 km/s |
| Age | 5.54±2.79 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
Omicron Coronae Borealis, Latinized from o Coronae Borealis, is a star in the northern constellation of Corona Borealis. It is a faint star but visible to the naked eye on a dark night with an apparent visual magnitude of +5.53.[2] The annual parallax shift of the star as seen from Earth is 12.08 mas, which provides a distance estimate of around 270 light years. It is moving closer to the Sun with a radial velocity of −54 km/s.[4]
Based upon the spectrum of this star, it has a stellar classification of K0 III.[3] This indicates this is an evolved K-type giant star that has exhausted the hydrogen at its core and has left the main sequence. This is a red clump star, which means it is now generating energy through helium fusion at its core. It has 107% of the mass of the Sun and has expanded to over ten times the Sun's radius. The star is radiating 50 times the Sun's luminosity from its expanded photosphere at an effective temperature of 4,812 K.[5]
Planetary system
Omicron Coronae Borealis has one confirmed planet, believed to be, along with HD 100655 b, one of the two least massive planets known around red clump giants.[5] The planet was detected by measuring changes in radial velocity of the host star caused by gravitational perturbation of the orbiting object. It is orbiting with a period of 188 days, at a semimajor axis 83% of the mean separation between the Earth and the Sun, and an eccentricity of 0.19.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >1.5 MJ | 0.83 | 187.83 ± 0.54 | 0.191 ± 0.085 | — | — |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.Vizier catalog entry
- ↑ 2.0 2.1 2.2 2.3 Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants", Monthly Notices of the Royal Astronomical Society 172 (3): 667–679, doi:10.1093/mnras/172.3.667, Bibcode: 1975MNRAS.172..667J.
- ↑ 3.0 3.1 3.2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 4.0 4.1 4.2 Jofré, E et al. (2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics 574: A50, doi:10.1051/0004-6361/201424474, A50, Bibcode: 2015A&A...574A..50J.
- ↑ 5.0 5.1 5.2 5.3 Sato, Bun'ei et al. (2012), "Substellar Companions to Seven Evolved Intermediate-Mass Stars", Publications of the Astronomical Society of Japan 64 (6): 135, doi:10.1093/pasj/64.6.135, Bibcode: 2012PASJ...64..135S, https://academic.oup.com/pasj/article/64/6/135/1422181.
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