Astronomy:Omega1 Aquarii

From HandWiki
Short description: Binary star in the constellation Aquarius


For other stars with this Bayer designation, see ω Aquarii.
Omega1 Aquarii
Location of ω1 Aquarii (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aquarius[1]
Right ascension  23h 39m 47.069s[2]
Declination −14° 13′ 19.75″[2]
Apparent magnitude (V) 4.96[3]
Characteristics
Evolutionary stage Main sequence[4]
Spectral type A7 IV[5] (A3V + K2V)[4]
B−V color index +0.25[3]
Astrometry
Radial velocity (Rv)–2[6] km/s
Proper motion (μ) RA: +50.434[2] mas/yr
Dec.: −49.097[2] mas/yr
Parallax (π)24.9012 ± 0.6158[2] mas
Distance131 ± 3 ly
(40.2 ± 1.0 pc)
Absolute magnitude (MV)+1.78[1]
Details
ω1 Aqr
Mass1.88±0.04 M☉[7]
1.72[4] M☉
Radius2.05[4] R☉
Luminosity17.5±1.8[4] L☉
Surface gravity (log g)3.88[8] cgs
Temperature7,516±52[4] K
Metallicity [Fe/H]−0.07[8] dex
Rotational velocity (v sin i)105[4] km/s
Age790 Myr[9]
600[10] Myr
ω1 Aqr B
Mass0.85[4] M☉
Radius0.77[4] R☉
Other designations
ω1 Aqr, 102 Aquarii, BD−15 6471, GC 32873, HD 222345, HIP 116758, HR 8968, SAO 165818, PPM 241928[11]
Database references
SIMBADdata

Omega1 Aquarii is a binary star system in the equatorial constellation of Aquarius. Its name is a Bayer designation that is Latinized from ω1 Aquarii, and abbreviated Omega1 Aqr or ω1 Aqr. With an apparent visual magnitude of 4.96,[3] this star is faintly visible to the naked eye in skies not significantly affected by light pollution. The distance to this star can be estimated from the parallax as approximately 138 light-years (42 parsecs).[2]

The stellar classification of this star is A3V,[4] matching an A-type main-sequence star. The star is about 600[10] million years old and is spinning rapidly with a projected rotational velocity of 105 km/s.[12] It has 1.9[7] times the mass of the Sun and 2.0[4] times the Sun's radius. Omega1 Aquarii is radiating 17.5[4] times the Sun's luminosity from its photosphere at an effective temperature of 7,516 K.[4]

Previously thought to be a single star,[9] in 2022 it was discovered to have a smaller companion, making it a binary star system. The secondary cmponent has a class of K2V, matching a K-type main sequence star with 85% of the mass and 77% of the radius of the Sun. It has a projected physical separation of about 1 astronomical unit from the primary star, and their predicted orbital period is 239 days. [4]

References

  1. ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 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 Corben, P. M.; Stoy, R. H. (1968), "Photoelectric Magnitudes and Colours for Bright Southern Stars", Monthly Notes of the Astronomical Society of Southern Africa 27: 11, Bibcode: 1968MNSSA..27...11C. 
  4. ↑ 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 4.10 4.11 4.12 4.13 Waisberg, Idel et al. (2023), "Binarity and beyond in a stars – I. Survey description and first results of VLTI/GRAVITY observations of VAST targets with high Gaia–Hipparcos accelerations", Monthly Notices of the Royal Astronomical Society 521 (4): 5232–5254, doi:10.1093/mnras/stad872, Bibcode: 2023MNRAS.521.5232W. 
  5. ↑ Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode: 1988mcts.book.....H. 
  6. ↑ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Washington: Carnegie Institution of Washington), Bibcode: 1953GCRV..C......0W. 
  7. ↑ 7.0 7.1 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. 
  8. ↑ 8.0 8.1 Takeda, Yoichi et al. (October 2018), "Photospheric carbon, nitrogen, and oxygen abundances of A-type main-sequence stars*", Publications of the Astronomical Society of Japan 70 (5): 91, doi:10.1093/pasj/psy091, 91, Bibcode: 2018PASJ...70...91T. 
  9. ↑ 9.0 9.1 De Rosa, R. J. et al. (2014), "The VAST Survey - III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society 437 (2): 1216–1240, doi:10.1093/mnras/stt1932, Bibcode: 2014MNRAS.437.1216D. 
  10. ↑ 10.0 10.1 Vican, Laura (June 2012), "Age Determination for 346 Nearby Stars in the Herschel DEBRIS Survey", The Astronomical Journal 143 (6): 135, doi:10.1088/0004-6256/143/6/135, Bibcode: 2012AJ....143..135V. 
  11. ↑ "* ome01 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+ome01+Aqr. 
  12. ↑ Royer, F. et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics 463 (2): 671–682, doi:10.1051/0004-6361:20065224, Bibcode: 2007A&A...463..671R. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Omega1_Aquarii&oldid=3932699"