Omicron2 Cancri
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Cancer |
| Right ascension | 08h 57m 35.200s[2] |
| Declination | +15° 34′ 52.63″[2] |
| Apparent magnitude (V) | +5.67[3] |
| Characteristics | |
| Evolutionary stage | Subgiant[4] |
| Spectral type | F0 IV[5][4] |
| B−V color index | +0.204[3] |
| Astrometry | |
| Radial velocity (Rv) | −1.71±0.18[6] km/s |
| Proper motion (μ) | RA: +60.077 mas/yr[2] Dec.: +20.781 mas/yr[2] |
| Parallax (π) | 20.4546±0.0523 mas[2] |
| Distance | 159.5 ± 0.4 ly (48.9 ± 0.1 pc) |
| Absolute magnitude (MV) | +2.58[7] |
| Details[4] | |
| Mass | 1.72±0.01 M☉ |
| Radius | 1.62±0.08 R☉ |
| Luminosity | 10.30±0.43 L☉ |
| Surface gravity (log g) | 4.25 cgs |
| Temperature | 7,868 K |
| Metallicity [Fe/H] | 0.2 dex |
| Rotational velocity (v sin i) | 90.5±4.5[7] km/s |
| Age | 300[8] Myr |
| Other designations | |
| ο2 Cnc, 63 Cancri, BD+16°1864, GC 12380, HD 76582, HIP 44001, HR 3565, SAO 98250[9] | |
| Database references | |
| SIMBAD | data |
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Omicron2 Cancri is a solitary,[10] yellow-white-hued star in the zodiac constellation of Cancer. Its name is a Bayer designation that is Latinized from ο2 Cancri, and abbreviated Omicron2 Cnc or ο2 Cnc. With an apparent visual magnitude of +5.67,[3] it is dimly visible to the naked eye on a dark night. Based upon an annual parallax shift of 20.45 mas as seen from Earth,[2] this star is located around 150 light-years from the Sun. It most likely forms a co-moving pair with Omicron1 Cancri.[11]
With a stellar classification of F0 IV,[5] this presents as an F-type subgiant star that has left the main sequence and is evolving toward the giant stage. It is estimated to be roughly 300[8] million years old with a relatively high rotation rate, as shown by a projected rotational velocity of around 90.5 km/s.[7] With 1.72 times the mass of the Sun and 1.62 times the Sun's radius, it is radiating 10.3 times the solar luminosity from its photosphere at an effective temperature of 7,868 K.[4]
The star has an infrared excess, suggesting it surrounded by a circumstellar debris disk.[8] Modelling of this structure indicates there are three distinct components, consisting of belts orbiting at distances of about 20 AU, 80 AU and 270 AU from the central star. They are inclined at an angle of 64° to the line of sight along a position angle of 103°. The gaps between the belts are most likely maintained by orbiting planets.[4]
References
[edit]- ^ Matrà, L.; et al. (January 15, 2025), "REsolved ALMA and SMA Observations of Nearby Stars (REASONS): A population of 74 resolved planetesimal belts at millimetre wavelengths", Astronomy and Astrophysics, 693, arXiv:2501.09058, Bibcode:2025A&A...693A.151M, doi:10.1051/0004-6361/202451397.
- ^ 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 c d e Marshall, Jonathan P.; et al. (July 2016), "Far-infrared and sub-millimetre imaging of HD 76582's circumstellar disc", Monthly Notices of the Royal Astronomical Society, 459 (3): 2893–2904, arXiv:1604.08306, Bibcode:2016MNRAS.459.2893M, doi:10.1093/mnras/stw813.
- ^ 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.
- ^ Gaia Collaboration (May 2022), "Gaia Data Release 3 (Gaia DR3). Part 1. Main source", VizieR On-line Data Catalog: I/355. Originally published in: doi:10.1051/0004-63, Bibcode:2022yCat.1355....0G, doi:10.26093/cds/vizier.1355.
- ^ a b c Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics, 446 (1): 267–277, arXiv:astro-ph/0509399, Bibcode:2006A&A...446..267R, doi:10.1051/0004-6361:20053911, S2CID 8642707.
- ^ 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.
- ^ "omi02 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-06-14.
{{cite web}}: CS1 maint: postscript (link) - ^ 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.
