Xi Aurigae

Xi Aurigae
Location of ξ Aurigae (circled in red)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Auriga[1]
Right ascension 05h 54m 50.76694s[2]
Declination +55° 42′ 25.0802″[2]
Apparent magnitude (V) +5.00[3]
Characteristics
Evolutionary stage main sequence[4]
Spectral type A2 Va[5]
U−B color index +0.12[3]
B−V color index +0.05[3]
Astrometry
Radial velocity (Rv)−13.3±2.4[6] km/s
Proper motion (μ) RA: −7.049 mas/yr[2]
Dec.: +12.959 mas/yr[2]
Parallax (π)13.3702±0.1670 mas[2]
Distance244 ± 3 ly
(74.8 ± 0.9 pc)
Absolute magnitude (MV)+0.64[1]
Details
Mass2.26[7] M☉
Radius2.86[7] R☉
Luminosity47.3[7] L☉
Surface gravity (log g)3.88[7] cgs
Temperature8,954[7] K
Metallicity [Fe/H]−0.36±0.04[1] dex
Rotational velocity (v sin i)62[8] km/s
Age174[8] Myr
Other designations
ξ Ari, 30 Aurigae, BD+55°1027, FK5 1157, GC 7404, HD 39283, HIP 27949, HR 2029, SAO 25450, PPM 30117[9]
Database references
SIMBADdata

Xi Aurigae is a single,[10] white-hued star in the northern constellation of Auriga. Its name is a Bayer designation that is Latinized from ξ Aurigae, and abbreviated Xi Aur or ξ Ari. This star was once considered part of the constellation of Camelopardalis and held the Flamsteed designation 32 Camelopardalis.[11] It is visible to the naked eye with an apparent visual magnitude of +5.0.[3] The measured annual parallax shift of this star is 13.37 mas,[2] which corresponds to a physical distance of 244 light-years (75 parsecs) with a 3 light-year margin of error. At that distance, the visual magnitude of the star is diminished by an extinction of 0.108 due to interstellar dust.[12] The star is drifting closer to the Sun with a radial velocity of −13 km/s.[6]

This is an A-type main sequence star with a stellar classification of A2 Va.[5] Although it was one of the first stars to be cataloged as a Lambda Boötis star, Murphy et al. (2015) don't consider it to be a member of this population.[5] The star has nearly twice[8] the mass of the Sun and about 2.9 times the Sun's radius.[7] It is an estimated 174 million years old[8] and is spinning with a projected rotational velocity of 62 km/s.[7] Xi Aurigae is radiating 47.3 times the Sun's luminosity from its photosphere at an effective temperature of around 8,954 K.[7]

References

  1. 1 2 3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 4 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.
  4. ↑ Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691.
  5. 1 2 3 Murphy, Simon J.; et al. (October 2015), "An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue", Publications of the Astronomical Society of Australia, 32: 43, arXiv:1508.03633, Bibcode:2015PASA...32...36M, doi:10.1017/pasa.2015.34, S2CID 59405545, e036.
  6. 1 2 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  7. 1 2 3 4 5 6 7 8 Stassun, Keivan G.; et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467.
  8. 1 2 3 4 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. ↑ "ksi Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-28.
  10. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  11. ↑ Wagman, M. (August 1987), "Flamsteed's Missing Stars", Journal for the History of Astronomy, 18 (3): 213, Bibcode:1987JHA....18..209W, doi:10.1177/002182868701800305, S2CID 118445625.
  12. ↑ Murphy, Simon J.; Paunzen, Ernst (April 2017), "Gaia's view of the λ Boo star puzzle", Monthly Notices of the Royal Astronomical Society, 466 (1): 546–555, arXiv:1612.01528, Bibcode:2017MNRAS.466..546M, doi:10.1093/mnras/stw3141, S2CID 119328659.
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