Astronomy:14 Aurigae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Auriga |
| Right ascension | 05h 15m 24.39398s[2] |
| Declination | +32° 41′ 15.3638″[2] |
| Apparent magnitude (V) | 5.01[3] (5.08 + 7.86)[4] |
| Characteristics | |
| Spectral type | A9IV + ? + F5V + M3V: + WDA[4] |
| U−B color index | +0.19[5] |
| B−V color index | +0.222±0.004[3] |
| Variable type | δ Scuti[6] |
| Astrometry | |
| Radial velocity (Rv) | −9.3±0.2[3] km/s |
| Proper motion (μ) | RA: −25.062[2] mas/yr Dec.: +12.056[2] mas/yr |
| Parallax (π) | 12.1306 ± 0.1712[2] mas |
| Distance | 269 ± 4 ly (82 ± 1 pc) |
| Absolute magnitude (MV) | 0.31[3] |
| Details | |
| 14 Aur Aa | |
| Mass | 1.64[7] M☉ |
| Luminosity | 62.07[3] L☉ |
| Surface gravity (log g) | 3.46[8] cgs |
| Temperature | 7,498[8] K |
| Metallicity [Fe/H] | −0.02[3] dex |
| Rotation | 2.11 h[6] |
| Rotational velocity (v sin i) | 27.6[8] km/s |
| Age | 609[7] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
14 Aurigae is a quadruple star system located 269[2] light years away from the Sun in the zodiac constellation of Auriga. It has the variable star designation KW Aurigae, whereas 14 Aurigae is the Flamsteed designation.[9] It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.01.[3] The system is moving closer to the Sun with a heliocentric radial velocity of −9 km/s.[3]
The magnitude 5.08[4] primary member, designated component A, is a single-lined spectroscopic binary system in a circular orbit with a period of 3.7887 days.[10] The visible member has a stellar classification of A9 IV or A V, depending on the source,[11] and is a Delta Scuti variable with an amplitude of 0.08 magnitude and a period of 2.11 hours.[6] It is 609 million years old with 1.64 times the mass of the Sun.[7]
Component B lies about 10″ to the north of the primary and is merely a visual companion. However, component C, an F-type main sequence star of magnitude 7.86,[4] shares a common proper motion with component A and thus they form a system. This member is also a single-lined spectroscopic binary, having a period of 2.9934 days. The final member of the system, now designated component Cb, is a white dwarf star that is separated from the C, or rather Ca pair by 2″. If it is indeed bound to Ca, its orbital period is around 1,300 years.[11]
References
- ↑ Fitch, W. S.; Wisniewski, W. Z. (August 1979). "Tidal effects in pulsating stars. III. l = 1 p5-modes in the ellipsoidal variable 14 Aurigae A". The Astrophysical Journal 231: 808–825. doi:10.1086/157246. Bibcode: 1979ApJ...231..808F. https://ui.adsabs.harvard.edu/abs/1979ApJ...231..808F. Retrieved 29 October 2021.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 4.0 4.1 4.2 4.3 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E
- ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M.
- ↑ 6.0 6.1 6.2 Solano, E.; Fernley, J. (April 1997). "Spectroscopic survey of delta Scuti stars. I. Rotation velocities and effective temperatures". Astronomy & Astrophysics Supplement Series 122: 131–147. doi:10.1051/aas:1997329. Bibcode: 1997A&AS..122..131S.
- ↑ 7.0 7.1 7.2 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.
- ↑ 8.0 8.1 8.2 Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo", Astronomy and Astrophysics 493 (3): 1099–1107, doi:10.1051/0004-6361:200810377, Bibcode: 2009A&A...493.1099S, http://goedoc.uni-goettingen.de/goescholar/bitstream/handle/1/9690/aa10377-08.pdf?sequence=2[yes|permanent dead link|dead link}}]
- ↑ 9.0 9.1 "14 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=14+Aur.
- ↑ Pourbaix, D. et al. (2004). "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits". Astronomy & Astrophysics 424: 727–732. doi:10.1051/0004-6361:20041213. Bibcode: 2004A&A...424..727P.
- ↑ 11.0 11.1 Barstow, M. A. et al. (April 2001). "Resolving Sirius-like binaries with the Hubble Space Telescope". Monthly Notices of the Royal Astronomical Society 322 (4): 891–900. doi:10.1046/j.1365-8711.2001.04203.x. Bibcode: 2001MNRAS.322..891B.
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