14 Aurigae

Quadruple star system in the constellation Auriga Auriga constellation map.svg center 280 right Red circle.svg 10 14 Aurigae 618 645 Location of 14 Aurigae (circled in red) J2000 05 15 24.39420 +32 41 15.3597 5.01 (5.08 + 7.86) Auriga A9IV + ? + F5V + M3V: + WDA +0.222 0.004 +0.19 δ Scuti −9.3 0.2 −25.256 0.121 +12.339 0.087 12.0126 0.1151 0.31 14 Aur Aa 1.64 62.07 7,498 3.46 −0.02 2.11 h 27.6 609 KW Aurigae 14 Aur 3824 +32°492 +32 922 1 J05154+3242 6411 3112 02394-02028 +32°922 33959 24504 1706 PPM+70096 746 4235 2394-2028-1 57799 213 5004 14+Aur 14 Aurigae is a quadruple star system located 272 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. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.01. The system is moving closer to the Sun with a heliocentric radial velocity of −9 km/s. thumb|left|A visual band light curve for 14 Aurigae, adapted from Fitch and Wisniewski (1979) The magnitude 5.08 primary member, designated component A, is a single-lined spectroscopic binary system in a circular orbit with a period of 3.7887 days. The visible member has a stellar classification of A9 IV or A V, depending on the source. In 1966, Ivan John Danziger and Robert John Dickens discovered that 14 Aurigae star is a variable star. It is a Delta Scuti variable with an amplitude of 0.08 magnitude and a period of 2.11 hours. It is 609 million years old with 1.64 times the mass of the Sun. Component B lies about 10 arcsecond 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, 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 arcsecond. While it is statistically unlikely that a chance alignment between Cb and the rest of the system would occur, it has not been proven whether Cb is a physical companion of Ca. If Cb is indeed bound to Ca, which would make 14 Aurigae a quintuple system, its orbital period is around 1,300 years. References Fitch W. S. Wisniewski W. Z. Tidal effects in pulsating stars. III. l = 1 p5-modes in the ellipsoidal variable 14 Aurigae A The Astrophysical Journal August 1979 231 808–825 10.1086/157246 1979ApJ...231..808F https://ui.adsabs.harvard.edu/abs/1979ApJ...231..808F 29 October 2021 180702438220217344 14 Aur 2019-05-20 Danziger I. J. Dickens R. J. Observations of Variable F-Type Stars with Short Periods Information Bulletin on Variable Stars August 1966 150 1 1966IBVS..150....1D https://ibvs.konkoly.hu/pub/ibvs/0101/0150.pdf 29 November 2024 Eggleton P. P. Tokovinin A. A. A catalogue of multiplicity among bright stellar systems Monthly Notices of the Royal Astronomical Society 389 2 869–879 September 2008 10.1111/j.1365-2966.2008.13596.x free 2008MNRAS.389..869E 0806.2878 14878976 XHIP: An extended hipparcos compilation Anderson E. Francis Ch. Astronomy Letters 38 5 331 2012 2012AstL...38..331A 1108.4971 10.1134/S1063773712050015 119257644 Spectroscopic survey of delta Scuti stars. I. Rotation velocities and effective temperatures Solano E. Fernley J. Astronomy & Astrophysics Supplement Series 122 131–147 April 1997 10.1051/aas:1997329 1997A&AS..122..131S free Mermilliod J.-C. Compilation of Eggen's UBV data, transformed to UBV (unpublished) Catalogue of Eggen's UBV Data 1986 1986EgUBV........0M Schröder C. Reiners Ansgar Schmitt Jürgen H. M. M. Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo Astronomy and Astrophysics 493 3 1099–1107 January 2009 10.1051/0004-6361:200810377 2009A&A...493.1099S free http://goedoc.uni-goettingen.de/goescholar/bitstream/handle/1/9690/aa10377-08.pdf?sequence=2 2021-09-11 2017-09-22 https://web.archive.org/web/20170922162905/https://goedoc.uni-goettingen.de/bitstream/handle/1/9690/aa10377-08.pdf?sequence=2 dead Resolving Sirius-like binaries with the Hubble Space Telescope Barstow M. A. Bond Howard E. Burleigh M. R. Holberg J. B. Monthly Notices of the Royal Astronomical Society 322 4 891–900 April 2001 1 10.1046/j.1365-8711.2001.04203.x free astro-ph/0010645 2001MNRAS.322..891B 12232120 1 Pourbaix D. Tokovinin A. A. Batten A. H. Fekel F. C. Hartkopf W. I. Levato H. Morrell N. I. Torres G. Udry S. 2004 727–732 424 SB9: The Ninth Catalogue of Spectroscopic Binary Orbits Astronomy & Astrophysics 2004A&A...424..727P 10.1051/0004-6361:20041213 free astro-ph/0406573 119387088 David Trevor J. Hillenbrand Lynne A. 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 2015 2015ApJ...804..146D 10.1088/0004-637X/804/2/146 1501.03154 33401607 External links HR 1706 CCDM J05154+3242 Image 14 Aurigae Category:A-type main-sequence stars Category:White dwarfs Category:Quadruple star systems Category:Delta Scuti variables Category:Auriga BD+32 0922 Aurigae, 14 033959 024504 1706 Aurigae, KW Category:A9IV stars Category:F5V stars Category:M3V stars