Astronomy:Omicron2 Cancri

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Short description: Star in the constellation Cancer


For other stars with this Bayer designation, see ο Cancri.
Omicron2 Cancri
The 74 exocomet belts imaged by ALMA’s REASONS survey, showing belts of all shapes, sizes and ages (REASONS comboplot full nonames).jpg
Image of the debris disk with the REASONS survey[1]
Observation data
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 main sequence[2][4]
Spectral type F0 IV[5][6]
B−V color index +0.204[3]
Astrometry
Radial velocity (Rv)−1.71±0.18[7] km/s
Proper motion (μ) RA: +60.077[2] mas/yr
Dec.: +20.781[2] mas/yr
Parallax (π)20.4546 ± 0.0523[2] mas
Distance159.5 ± 0.4 ly
(48.9 ± 0.1 pc)
Absolute magnitude (MV)+2.58[8]
Details
Mass1.72±0.01[6] M☉
Radius1.62±0.08[6] R☉
Luminosity10.30±0.43[6] L☉
Surface gravity (log g)4.25[6] cgs
Temperature7,868[6] K
Metallicity [Fe/H]+0.2[6] dex
Rotational velocity (v sin i)90.5±4.5[8] km/s
Age300[9] Myr
Other designations
ο2 Cnc, 63 Cancri, BD+16°1864, GC 12380, HD 76582, HIP 44001, HR 3565, SAO 98250[10]
Database references
SIMBADdata

Omicron2 Cancri is a solitary,[11] 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.[12]

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. Other authors give it a spectral class of A7V[13] and evolutionary models place it on the main sequence.[4][2] It is estimated to be roughly 300[9] million years old with a relatively high rotation rate, as shown by a projected rotational velocity of around 90.5 km/s.[8] 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.[6]

The star has an infrared excess, suggesting it surrounded by a circumstellar debris disk.[9] 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.[6]

References

  1. ↑ 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, doi:10.1051/0004-6361/202451397, Bibcode: 2025A&A...693A.151M. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940.  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 Häggkvist, L.; Oja, T. (1966), "Photoelectric photometry of bright stars", Arkiv för Astronomi 4: 137–163, Bibcode: 1966ArA.....4..137H. 
  4. ↑ 4.0 4.1 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. Bibcode: 2012A&A...537A.120Z. 
  5. ↑ 5.0 5.1 Cowley, A. et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, doi:10.1086/110819, Bibcode: 1969AJ.....74..375C. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 6.8 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, doi:10.1093/mnras/stw813, Bibcode: 2016MNRAS.459.2893M. 
  7. ↑ 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, doi:10.26093/cds/vizier.1355, Bibcode: 2022yCat.1355....0G. 
  8. ↑ 8.0 8.1 8.2 Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics 446 (1): 267–277, doi:10.1051/0004-6361:20053911, Bibcode: 2006A&A...446..267R. 
  9. ↑ 9.0 9.1 9.2 Rhee, Joseph H. et al. (May 2007), "Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs", The Astrophysical Journal 660 (2): 1556–1571, doi:10.1086/509912, Bibcode: 2007ApJ...660.1556R. 
  10. ↑ "omi02 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=omi02+Cnc. 
  11. ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  12. ↑ 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, doi:10.1088/0067-0049/192/1/2, 2, Bibcode: 2011ApJS..192....2S. 
  13. ↑ Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement Series 99: 135, doi:10.1086/192182, Bibcode: 1995ApJS...99..135A 



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