Xi Arietis

Xi Arietis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Aries
Right ascension 02h 24m 49.05655s[1]
Declination +10° 36′ 38.0236″[1]
Apparent magnitude (V) +5.46[2]
Characteristics
Spectral type B7 IV[3]
U−B color index −0.48[2]
B−V color index −0.10[2]
Astrometry
Proper motion (μ) RA: +20.09[1] mas/yr
Dec.: −14.79[1] mas/yr
Parallax (π)3.74 ± 0.29 mas[1]
Distance870 ± 70 ly
(270 ± 20 pc)
Absolute magnitude (MV)−0.43[4]
Details
Mass3.9[5] M☉
Surface gravity (log g)3.897±0.017[5] cgs
Temperature13627±100[5] K
Rotational velocity (v sin i)164±8[5] km/s
Age195[4] Myr
Other designations
ξ Ari, ψ Ceti, 24 Arietis, BD+09°316, FK5 2164, HD 14951, HIP 11249, HR 702, SAO 92932[6]
Database references
SIMBADdata

Xi Arietis, Latinized from ξ Arietis, is the Bayer designation for a binary star[7] system in the northern constellation of Aries. It has an apparent visual magnitude of 5.46,[2] and so is dimly visible to the naked eye. Based upon an annual parallax shift of 3.74±0.29 mas as seen from Earth, it is 872 ± 68 light-years (267 ± 21 parsecs) distant from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.24 due to interstellar dust.[4]

This is a double-lined spectroscopic binary.[7] The spectrum matches a stellar classification of B7 IV,[3] which would indicate a subgiant star that has exhausted the supply of hydrogen at its core and is in the process of evolving into a giant star. Xi Arietis was once a designation for Psi Ceti (ψ Cet, ψ Ceti), and was later recognized to be a duplicate by Bayer.[8]

References

  1. ^ a b c d e van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c d Crawford, D. L.; et al. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode:1971AJ.....76.1058C, doi:10.1086/111220.
  3. ^ a b Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode:1968ApJS...17..371L, doi:10.1086/190179.
  4. ^ a b c Gontcharov, G. A. (November 2012), "Spatial distribution and kinematics of OB stars", Astronomy Letters, 38 (11): 694–706, arXiv:1606.09028, Bibcode:2012AstL...38..694G, doi:10.1134/S1063773712110035, S2CID 119108982.
  5. ^ a b c d Huang, Wenjin; et al. (October 2010), "A Stellar Rotation Census of B Stars: From ZAMS to TAMS", The Astrophysical Journal, 722 (1): 605–619, arXiv:1008.1761, Bibcode:2010ApJ...722..605H, doi:10.1088/0004-637X/722/1/605, S2CID 118532653.
  6. ^ "ksi Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-28.
  7. ^ a b Chini, R.; et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society, 424 (3): 1925, arXiv:1205.5238, Bibcode:2012MNRAS.424.1925C, doi:10.1111/j.1365-2966.2012.21317.x, S2CID 119120749.
  8. ^ Ridpath, Ian, "Bayer's Uranometria and Bayer letters", Star Tales.