Omicron1 Cancri
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Cancer[1] |
| Right ascension | 08h 57m 14.950s[2] |
| Declination | +15° 19′ 21.96″[2] |
| Apparent magnitude (V) | +5.20[3] |
| Characteristics | |
| Spectral type | A5 III[4] |
| B−V color index | +0.1540[3] |
| Astrometry | |
| Radial velocity (Rv) | −4.6±2.8[5] km/s |
| Proper motion (μ) | RA: +60.732 mas/yr[2] Dec.: +20.396 mas/yr[2] |
| Parallax (π) | 20.3294±0.0891 mas[2] |
| Distance | 160.4 ± 0.7 ly (49.2 ± 0.2 pc) |
| Absolute magnitude (MV) | +1.92[1] |
| Details | |
| Mass | 2.02[6] M☉ |
| Radius | 1.86[7] R☉ |
| Luminosity | 13.4[8] L☉ |
| Surface gravity (log g) | 3.982+0.008 −0.005[9] cgs |
| Temperature | 8,145±3[9] K |
| Metallicity [Fe/H] | −0.85+0.09 −0.04[9] dex |
| Rotational velocity (v sin i) | 90[6] km/s |
| Age | 598[6] Myr |
| Other designations | |
| ο1 Cnc, 62 Cancri, BD+15°1945, HD 76543, HIP 43970, HR 3561, SAO 98247[10] | |
| Database references | |
| SIMBAD | data |
Omicron1 Cancri is a solitary,[11] white-hued star in the zodiac constellation of Cancer. Its name is a Bayer designation that is Latinized from ο1 Cancri, and abbreviated Omicron1 Cancri or ο1 Cnc. This star is faintly visible to the naked eye with an apparent visual magnitude of +5.20.[3] Based upon an annual parallax shift of 20.33 mas as seen from Earth,[2] it is located 160 light-years (49 pc) away from the Sun. It most likely forms a co-moving pair with Omicron2 Cancri.[12]
With a stellar classification of A5 III,[4] this presents as an evolved, A-type giant star. At the age of about 600 million years,[6] it has double[6] the mass of the Sun and 1.86 times the Sun's radius.[7] Omicron1 Cancri is radiating 13.4[8] times the solar luminosity from its photosphere at an effective temperature of about 8,145 K.[9] It has a high rate of spin, showing a projected rotational velocity of 90 km/s.[13]
Omicron1 Cancri has an infrared excess, indicating it surrounded by a circumstellar debris disk.[7] The signature matches a two-component disk with the spatially separated belts having temperatures of 146 K and 81 K.[8]
References
[edit]- ^ a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015 XHIP record for this object at VizieR.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875 Gaia DR3 record for this source at VizieR.
- ^ a b c Häggkvist, L.; Oja, T. (1966), "Photoelectric photometry of bright stars", Arkiv för Astronomi, 4: 137–163, Bibcode:1966ArA.....4..137H.
- ^ a b Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
- ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- ^ a b c d e David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ a b c Rhee, Joseph H.; et al. (May 2007), "Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs", The Astrophysical Journal, 660 (2): 1556–1571, arXiv:astro-ph/0609555, Bibcode:2007ApJ...660.1556R, doi:10.1086/509912, S2CID 11879505.
- ^ a b c Vican, Laura; et al. (December 2016), "Herschel Observations of Dusty Debris Disks", The Astrophysical Journal, 833 (2): 19, arXiv:1607.03754, Bibcode:2016ApJ...833..263V, doi:10.3847/1538-4357/833/2/263, S2CID 119271799, 263.
- ^ a b c d Royer, P.; et al. (January 2024), "MELCHIORS. The Mercator Library of High Resolution Stellar Spectroscopy", Astronomy & Astrophysics, 681, id. A107, arXiv:2311.02705, Bibcode:2024A&A...681A.107R, doi:10.1051/0004-6361/202346847.
- ^ "omi01 Cnc", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-06-15.
- ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Shaya, Ed J.; Olling, Rob P. (January 2011), "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalogue", The Astrophysical Journal Supplement, 192 (1): 17, arXiv:1007.0425, Bibcode:2011ApJS..192....2S, doi:10.1088/0067-0049/192/1/2, S2CID 119226823, 2.
- ^ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
