54 Aurigae is a multiple star system located around 800 light-years (51,000,000 AU) away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, blue-white hued star with a combined apparent visual magnitude of 6.02.[5] The system is moving further from the Sun with a heliocentric radial velocity of around +19 km/s.[5]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| A | |
| Right ascension | 06h 39m 33.12003s[2] |
| Declination | +28° 15′ 47.2764″[2] |
| Apparent magnitude (V) | 6.22[3] |
| B | |
| Right ascension | 06h 39m 33.11965s[2] |
| Declination | +28° 15′ 47.2740″[2] |
| Apparent magnitude (V) | 7.82[3] |
| Characteristics | |
| Spectral type | B7 III[4] |
| B−V color index | −0.087±0.007[5] |
| Variable type | Algol[6] |
| Astrometry | |
| A | |
| Radial velocity (Rv) | +19.0±4.3[5] km/s |
| Proper motion (μ) | RA: −5.461[2] mas/yr Dec.: −10.523[2] mas/yr |
| Parallax (π) | 3.5961 ± 0.0952 mas[2] |
| Distance | 910 ± 20 ly (278 ± 7 pc) |
| Details | |
| 54 Aur A | |
| Luminosity | 315.49[7] L☉ |
| Temperature | 11,083[7] K |
| Rotational velocity (v sin i) | 65[8] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
54 Aurigae is resolved into two visible components, of magnitudes 6.22 and 7.82, separated by 0.8″. The double was discovered in 1843 when the separation was only 0.7″.[10] There is no separate measure of the parallax of the secondary, but it shares a common proper motion with the brighter star[11] and they are assumed to form a binary.[10] The spectral class B7 III is assigned to the brighter of the pair, indicating a hot giant star, although it has also been given as B7/8 III/V, suggesting it may be a main sequence star.[12] Most sources can't give a separate spectral classification for the fainter star, but it has been listed as DA1/K4V, indicating it is either a white dwarf or red dwarf.[13]
The brighter component of the visible pair is an eclipsing binary with a period of 1.8797 days, and a primary eclipse depth of 0.03 magnitudes.[14] It is radiating 315 times the luminosity of the Sun from its photosphere at an effective temperature of 11,083 K (10,810 °C; 19,490 °F),[7] and is spinning with a projected rotational velocity of 65 kilometres per second (40 mi/s).[8]
References edit
- ^ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 7 October 2022.
- ^ a b c d e f g 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 Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Cucchiaro, A.; et al. (October 1977), "Spectral classification from the ultraviolet line features of S2/68 spectra. II - Late B-type stars", Astronomy and Astrophysics Supplement Series, 30: 71–79, Bibcode:1977A&AS...30...71C.
- ^ 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.
- ^ "NSV 3065", The International Variable Star Index, AAVSO, retrieved 7 October 2022.
- ^ a b c McDonald, I.; et al. (2012), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–357, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
- ^ a b Abt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590
- ^ "54 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-24.
- ^ a b Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (December 2001), "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920, ISSN 0004-6256.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Clausen, J. V.; Jensen, K. S. (1979), "Classification Based on 102/A/Mm Objective Prism Spectra", IAU Colloq. 47: Spectral Classification of the Future, 9: 479, Bibcode:1979RA......9..479C.
- ^ Pickles, A.; Depagne, É. (2010), "All-Sky Spectrally Matched UBVRI - ZY and u′ g′ r′ i′ z′ Magnitudes for Stars in the Tycho2 Catalog", Publications of the Astronomical Society of the Pacific, 122 (898): 1437, arXiv:1011.2020, Bibcode:2010PASP..122.1437P, doi:10.1086/657947, S2CID 54678796.
- ^ Wraight, K. T.; White, Glenn J.; Bewsher, D.; Norton, A. J. (October 2011), "STEREO observations of stars and the search for exoplanets", Monthly Notices of the Royal Astronomical Society, 416 (4): 2477–2493, arXiv:1103.0911, Bibcode:2011MNRAS.416.2477W, doi:10.1111/j.1365-2966.2011.18599.x.