Omicron Capricorni

Omicron Capricorni
Location of ο Capricorni (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Capricornus
ο Cap A
Right ascension 20h 29m 53.909s[1]
Declination −18° 34′ 59.46″[1]
Apparent magnitude (V) +5.94[2]
ο Cap B
Right ascension 20h 29m 52.594s[3]
Declination −18° 35′ 10.90″[3]
Apparent magnitude (V) +6.74[2]
Characteristics
ο Cap A
Spectral type A1 V[4]
U−B color index +0.30[2]
B−V color index +0.08[2]
ο Cap B
Spectral type A7/8 V[4]
U−B color index +0.04[2]
B−V color index +0.22[2]
Astrometry
ο Cap A
Radial velocity (Rv)−12.4±1.3[5] km/s
Proper motion (μ) RA: +29.058 mas/yr[1]
Dec.: −81.326 mas/yr[1]
Parallax (π)14.0193±0.0402 mas[1]
Distance232.6 ± 0.7 ly
(71.3 ± 0.2 pc)
ο Cap B
Radial velocity (Rv)−9.1±0.6[5] km/s
Proper motion (μ) RA: +29.266 mas/yr[3]
Dec.: −81.577 mas/yr[3]
Parallax (π)14.0435±0.0266 mas[3]
Distance232.2 ± 0.4 ly
(71.2 ± 0.1 pc)
Details
ο Cap A
Mass1.96±0.09[6] M☉
Radius1.92+0.13
−0.15[6] R☉
Luminosity18.6[7] L☉
Surface gravity (log g)4.23[6] cgs
Temperature10,492±357[8] K
Metallicity [Fe/H]0.00+0.12
−0.11 dex
Rotational velocity (v sin i)276[9] km/s
Age118[8] Myr
ο Cap B
Mass1.34±0.24[7] M☉
Temperature7,762[7] K
Rotational velocity (v sin i)136[9] km/s
Other designations
ο Cap, 12 Cap, ADS 13902, CCDM J20299-1835[10]
ο Cap A: BD−19°5831, GC 28503, HD 195094, HIP 101123, HR 7830, SAO 163626[11]
ο Cap B: BD−19°5830, GC 28502, HD 195093, HIP 101120, HR 7829, SAO 163625[12]
Database references
SIMBADA
B

Omicron Capricorni is a wide binary star[13] system in the constellation Capricornus.[14] Its name is a Bayer designation that is Latinized from ο Capricorni, and abbreviated Omicron Cap or ο Cap. The brighter component has an apparent visual magnitude of +5.94,[2] which is near the lower limit on stellar brightness that still can be seen with the naked eye. Based upon an annual parallax shift of 14.02 mas as seen from Earth,[1] this system is located at a distance of 233 light-years (71 pc) from the Sun. The proximity of this system to the ecliptic means it is subject to lunar occultation.[15]

Large but uncertain discrepancies in the parallax measurements from Hipparcos may indicate, weakly, that there is a third, unseen companion in the system.[13]

Both visible components are white-hued A-type main-sequence stars.[4] The primary, component A, sometimes called ο1 Capricorni, has an apparent magnitude of +5.94, while the companion, component B or ο2 Capricorni, has an apparent magnitude of +6.74.[2] The two stars are currently separated by 21.91[13] arcseconds, corresponding to a projected separation of around 2,100 AU.[16] At the estimated age of around 118[8] million years old, both components are spinning rapidly: component A has a projected rotational velocity of 276 km/s, while component B is 136 km/s.[9]

References

  1. ^ 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.
  2. ^ a b c d e f g h Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  3. ^ a b c d 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.
  4. ^ a b c Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1988mcts.book.....H.
  5. ^ a b Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  6. ^ a b c Bochanski, John J.; et al. (April 2018), "Fundamental Properties of Co-moving Stars Observed by Gaia", The Astronomical Journal, 155 (4): 17, arXiv:1801.00537, Bibcode:2018AJ....155..149B, doi:10.3847/1538-3881/aaaebe, S2CID 119256051, 149.
  7. ^ a b c Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  8. ^ a b c 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.
  9. ^ a b c Royer, F.; et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298.
  10. ^ "omi Cap", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-08-31.
  11. ^ "omi Cap A", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-08-31.
  12. ^ "omi Cap B", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-08-31.
  13. ^ a b c 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.
  14. ^ Harvard College Observatory (1941), Sky and Telescope, Stanford University.
  15. ^ Eitter, J. J.; Beavers, W. I. (August 1977), "Lunar occultation summary. II", Astrophysical Journal, Supplemental Series, 34: 493–504, Bibcode:1977ApJS...34..493E, doi:10.1086/190460.
  16. ^ Abt, Helmut A. (August 1988), "Maximum Separations among Cataloged Binaries", Astrophysical Journal, 331: 922, Bibcode:1988ApJ...331..922A, doi:10.1086/166609.
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