42 Aurigae
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga[1] |
| Right ascension | 06h 17m 34.6466s[2] |
| Declination | +46° 25′ 26.229″[2] |
| Apparent magnitude (V) | 6.53[1] |
| Characteristics | |
| Evolutionary stage | main sequence[2][3] |
| Spectral type | F0 V[4] or A6 Vp(4481 wk)n[5] |
| Apparent magnitude (G) | 6.48[2] |
| B−V color index | 0.263±0.003[1] |
| Astrometry | |
| Radial velocity (Rv) | −12.0±1.0[6] km/s |
| Proper motion (μ) | RA: −43.563±0.034[2] mas/yr Dec.: +11.150±0.026[2] mas/yr |
| Parallax (π) | 13.1070±0.0288 mas[2] |
| Distance | 248.8 ± 0.5 ly (76.3 ± 0.2 pc) |
| Absolute magnitude (MV) | 2.27[1] |
| Details | |
| Mass | 1.70±0.02[3] M☉ |
| Radius | 2.10[7] R☉ |
| Luminosity | 11.2[7] L☉ |
| Surface gravity (log g) | 4.18±0.14[8] cgs |
| Temperature | 7,660±260[8] K |
| Rotational velocity (v sin i) | 228[3] km/s |
| Age | 1.042[8] Gyr |
| Other designations | |
| 42 Aur, BD+46°1122, HD 43244, HIP 29884, HR 2228, SAO 40999[9] | |
| Database references | |
| SIMBAD | data |
42 Aurigae is a star in the northern constellation of Auriga. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It has an apparent visual magnitude of 6.53,[1] which places it just below the visibility limit for normal eyesight under good seeing conditions. It displays an annual parallax shift of 13.107 mas, which yields a distance estimate of around 248.8 light years.[2] The star is moving closer to the Sun with a radial velocity of −12 km/s.[6] It is a member of the Ursa Major Moving Group of stars that share a common motion through space.[10]
The star was assigned a stellar classification of F0 V by Nancy Roman in 1949,[4] indicating it is an F-type main-sequence star. However, in 1995 Abt and Morrell catalogued it as class A6 Vp(4481 wk)n;[5] a somewhat hotter and more massive A-type main-sequence star that displays spectral peculiarities as well as nebulous lines brought about by rapid rotation. It is around a billion years old[8] with a high rate of spin, showing a projected rotational velocity of 228 km/s.[3] The star has an estimated 1.7[3] times the mass of the Sun and is radiating 10[1] times the Sun's luminosity from its photosphere at an effective temperature of around 7,660 K.[8]
References
- ^ a b c d e f 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.
- ^ a b c d e f g h 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 e Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789, A120.
- ^ a b Roman, Nancy Grace (September 1949), "The Ursa Major Group", Astrophysical Journal, 110: 205, Bibcode:1949ApJ...110..205R, doi:10.1086/145199.
- ^ a b Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
- ^ a b 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 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.
- ^ 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.
- ^ "42 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-07.
- ^ Chupina, N. V.; et al. (June 2006), "Kinematic structure of the corona of the Ursa Major flow found using proper motions and radial velocities of single stars", Astronomy and Astrophysics, 451 (3): 909–916, Bibcode:2006A&A...451..909C, doi:10.1051/0004-6361:20054009.