Xi Aurigae
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Auriga |
| Right ascension | 05h 54m 50.76694s[1] |
| Declination | +55° 42′ 25.0802″[1] |
| Apparent magnitude (V) | +5.00[2] |
| Characteristics | |
| Spectral type | A2 Va[3] |
| U−B color index | +0.12[2] |
| B−V color index | +0.05[2] |
| Astrometry | |
| Radial velocity (Rv) | −13.3±2.4[4] km/s |
| Proper motion (μ) | RA: −7.049[1] mas/yr Dec.: +12.959[1] mas/yr |
| Parallax (π) | 13.3702 ± 0.1670 mas[1] |
| Distance | 244 ± 3 ly (74.8 ± 0.9 pc) |
| Absolute magnitude (MV) | +0.64[5] |
| Details[6] | |
| Mass | 1.96 M☉ |
| Radius | 1.1[7] R☉ |
| Luminosity | 49.5[5] L☉ |
| Surface gravity (log g) | 3.88 cgs |
| Temperature | 9,152±311 K |
| Metallicity [Fe/H] | −0.36±0.04[5] dex |
| Rotational velocity (v sin i) | 62 km/s |
| Age | 174 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Xi Aurigae, Latinized from ξ Aurigae, is the Bayer designation for a single,[9] white-hued star in the northern constellation of Auriga. This star was once considered part of the constellation of Camelopardalis and held the Flamsteed designation 32 Camelopardalis.[10] It is visible to the naked eye with an apparent visual magnitude of +5.0.[2] The measured annual parallax shift of this star is 13.37 ± 0.17 mas,[1] 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.[11]
This is an A-type main sequence star with a stellar classification of A2 Va.[3] 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.[3] The star has nearly twice[6] the mass of the Sun and about 1.1[7] times the Sun's radius. It is an estimated 174[6] million years old and is spinning with a projected rotational velocity of 62 km/s.[6] Xi Aurigae is radiating 49.5[5] times the Sun's luminosity from its photosphere at an effective temperature of around 9,152 K.[6]
References
[edit]- ^ a b c d e f 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.
- ^ a b c d 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.
- ^ a b c 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.
- ^ 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.
- ^ a b c d 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, S2CID 119257644.
- ^ a b c d e 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.
- ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (Third ed.): 5211–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ "ksi Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-28.
- ^ 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.
- ^ 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.
- ^ 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.
