Astronomy:Xi Aurigae
| Observation data 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 | |
| Spectral type | A2 Va[4] |
| U−B color index | +0.12[3] |
| B−V color index | +0.05[3] |
| Astrometry | |
| Radial velocity (Rv) | −13.3±2.4[5] km/s |
| Proper motion (μ) | RA: −7.049[2] mas/yr Dec.: +12.959[2] mas/yr |
| Parallax (π) | 13.3702 ± 0.1670[2] mas |
| Distance | 244 ± 3 ly (74.8 ± 0.9 pc) |
| Absolute magnitude (MV) | +0.64[1] |
| Details[6] | |
| Mass | 1.96 M☉ |
| Radius | 1.1[7] R☉ |
| Luminosity | 49.5[1] L☉ |
| Surface gravity (log g) | 3.88 cgs |
| Temperature | 9,152±311 K |
| Metallicity [Fe/H] | −0.36±0.04[1] dex |
| Rotational velocity (v sin i) | 62 km/s |
| Age | 174 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Xi Aurigae is a single,[9] 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.[10] 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.[11] The star is drifting closer to the Sun with a radial velocity of −13 km/s.[5]
This is an A-type main sequence star with a stellar classification of A2 Va.[4] 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.[4] 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[1] times the Sun's luminosity from its photosphere at an effective temperature of around 9,152 K.[6]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. XHIP record for this object at VizieR.
- ↑ 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.
- ↑ 3.0 3.1 3.2 3.3 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.
- ↑ 4.0 4.1 4.2 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, doi:10.1017/pasa.2015.34, e036, Bibcode: 2015PASA...32...36M.
- ↑ 5.0 5.1 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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 6.0 6.1 6.2 6.3 6.4 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, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 7.0 7.1 Pasinetti Fracassini, L. E. et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics 367: 5211–524, doi:10.1051/0004-6361:20000451, Bibcode: 2001A&A...367..521P.
- ↑ "ksi Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=ksi+Aur.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Wagman, M. (August 1987), "Flamsteed's Missing Stars", Journal for the History of Astronomy 18 (3): 213, doi:10.1177/002182868701800305, Bibcode: 1987JHA....18..209W.
- ↑ 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, doi:10.1093/mnras/stw3141, Bibcode: 2017MNRAS.466..546M.
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