14 Aurigae
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas[2] |
| 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] In 1966, Ivan John Danziger and Robert John Dickens discovered that 14 Aurigae star is a variable star.[12] It 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
[edit]- ^ 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. Bibcode:1979ApJ...231..808F. doi:10.1086/157246. Retrieved 29 October 2021.
- ^ a b c d e f 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.
- ^ a b c d e f g h 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 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
- ^ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- ^ a b c 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. Bibcode:1997A&AS..122..131S. doi:10.1051/aas:1997329.
- ^ a b c 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 c 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" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377[permanent dead link]
- ^ a b "14 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-20.
- ^ Pourbaix, D.; et al. (2004). "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits". Astronomy & Astrophysics. 424: 727–732. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID 119387088.
- ^ a b 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. arXiv:astro-ph/0010645. Bibcode:2001MNRAS.322..891B. doi:10.1046/j.1365-8711.2001.04203.x. S2CID 12232120.
- ^ Danziger, I. J.; Dickens, R. J. (August 1966). "Observations of Variable F-Type Stars with Short Periods" (PDF). Information Bulletin on Variable Stars. 150: 1. Bibcode:1966IBVS..150....1D. Retrieved 29 November 2024.
