14 Aurigae

A visual band light curve for 14 Aurigae, adapted from Fitch and Wisniewski (1979)[1]
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]
Distance269 ± 4 ly
(82 ± 1 pc)
Absolute magnitude (MV)0.31[3]
Details
14 Aur Aa
Mass1.64[7] M☉
Luminosity62.07[3] L☉
Surface gravity (log g)3.46[8] cgs
Temperature7,498[8] K
Metallicity [Fe/H]−0.02[3] dex
Rotation2.11 h[6]
Rotational velocity (v sin i)27.6[8] km/s
Age609[7] Myr
Other designations
14 Aur, KW Aurigae, AG+32° 492, BD+32° 922, GC 6411, HD 33959, HIP 24504, HR 1706, SAO 57799, ADS 3824, CCDM J05154+3242, TYC 2394-2028-1, GCRV 3112, GSC 02394-02028[9]
Database references
SIMBADdata

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

  1. ↑ 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.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 4 5 6 7 8 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.
  4. 1 2 3 4 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
  5. ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  6. 1 2 3 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.
  7. 1 2 3 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.
  8. 1 2 3 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
  9. 1 2 "14 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-20.
  10. ↑ 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.
  11. 1 2 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.
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