14 Aurigae
{{Short description|Quadruple star system in the constellation Auriga}}
{{Starbox begin}}
{{Starbox image
| image = 250px
| caption = A visual band light curve for 14 Aurigae, adapted from Fitch and Wisniewski (1979)
}}
{{Starbox observe
| epoch = J2000
| dec = {{DEC|+32|41|15.3638}}
| appmag_v = 5.01 {{nowrap|(5.08 + 7.86)}}
| constell = Auriga
}}
{{Starbox character
| type =
| class = {{nowrap|A9IV + ? + F5V + M3V: + WDA}}
| variable = δ Scuti
}}
{{Starbox astrometry
| parallax = 12.1306
| p_error = 0.1712
}}
{{Starbox detail
| component1 = 14 Aur Aa
| radius =
}}
{{Starbox catalog
| names = {{odlist | V=KW Aurigae | F=14 Aur | ADS=3824 | AG=+32° 492 | CSI=+32 922 1 | CCDM=J05154+3242 | GC=6411 | GCRV=3112 | GSC=02394-02028 | BD=+32° 922 | HD=33959 | HIP=24504 | HR=1706 | PPM+70096 | ROT=746 | TD1=4235 | TYC=2394-2028-1 | SAO=57799 | SBC7=213 | UBV=5004 }}
}}
{{Starbox reference
| Simbad = 14+Aur
}}
{{Starbox end}}
14 Aurigae is a quadruple star system located 269 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.
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 {{Val|10|ul=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 {{Val|2|u=arcsecond}}. If it is indeed bound to Ca, its orbital period is around 1,300 years.
References
{{reflist|refs=
{{cite DR2|211805079552264832}}
{{cite simbad | title=14 Aur | access-date=2019-05-20 }}
| last1=Danziger | first1=I. J. | last2=Dickens | first2=R. J.
| title=Observations of Variable F-Type Stars with Short Periods | journal=Information Bulletin on Variable Stars
| date=August 1966 | volume=150 | page=1 | bibcode=1966IBVS..150....1D | url=https://ibvs.konkoly.hu/pub/ibvs/0101/0150.pdf
| access-date=29 November 2024}}
| last1=Eggleton | first1=P. P. | last2=Tokovinin | first2=A. A.
| title=A catalogue of multiplicity among bright stellar systems
| journal=Monthly Notices of the Royal Astronomical Society
| volume=389 | issue=2 | pages=869–879 | date=September 2008
| doi=10.1111/j.1365-2966.2008.13596.x
| doi-access=free | bibcode=2008MNRAS.389..869E | arxiv=0806.2878 | s2cid=14878976 }}
| title=XHIP: An extended hipparcos compilation
| last1=Anderson | first1=E. | last2=Francis | first2=Ch.
| journal=Astronomy Letters | volume=38 | issue=5 | pages=331 | year=2012
| bibcode=2012AstL...38..331A | arxiv=1108.4971
| doi=10.1134/S1063773712050015 | s2cid=119257644 }}
| title=Spectroscopic survey of delta Scuti stars. I. Rotation velocities and effective temperatures
| last1=Solano | first1=E. | last2=Fernley | first2=J.
| journal=Astronomy & Astrophysics Supplement Series | volume=122 | pages=131–147 | date=April 1997
| doi=10.1051/aas:1997329 | bibcode=1997A&AS..122..131S | doi-access=free }}
| last1=Mermilliod | first1=J.-C.
| title=Compilation of Eggen's UBV data, transformed to UBV (unpublished)
| journal=Catalogue of Eggen's UBV Data
| date=1986 | bibcode= 1986EgUBV........0M }}
| title=Resolving Sirius-like binaries with the Hubble Space Telescope
| last1=Barstow | first1=M. A. | last2=Bond | first2=Howard E.
| last3=Burleigh | first3=M. R. | last4=Holberg | first4=J. B.
| journal=Monthly Notices of the Royal Astronomical Society
| volume=322 | issue=4 | pages=891–900 | date=April 2001
| display-authors=1 | doi=10.1046/j.1365-8711.2001.04203.x
| doi-access=free | arxiv=astro-ph/0010645 | bibcode=2001MNRAS.322..891B | s2cid=12232120 }}
| display-authors=1 | last1=Pourbaix | first1=D.
| last2=Tokovinin | first2=A. A. | last3=Batten | first3=A. H.
| last4=Fekel | first4=F. C. | last5=Hartkopf | first5=W. I.
| last6=Levato | first6=H. | last7=Morrell | first7=N. I.
| last8=Torres | first8=G. | last9=Udry | first9=S.
| year=2004 | pages=727–732 | volume=424
| title=SB9: The Ninth Catalogue of Spectroscopic Binary Orbits
| journal=Astronomy & Astrophysics
| bibcode=2004A&A...424..727P | doi=10.1051/0004-6361:20041213 | arxiv=astro-ph/0406573 | s2cid=119387088 }}
| last1=David | first1=Trevor J. | last2=Hillenbrand | first2=Lynne A.
| title=The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets
| journal=The Astrophysical Journal
| volume=804 | issue=2 | pages=146 | year=2015
| bibcode=2015ApJ...804..146D | doi=10.1088/0004-637X/804/2/146
| arxiv=1501.03154 | s2cid=33401607 }}
}}
External links
- [http://webviz.u-strasbg.fr/viz-bin/VizieR-S?HR%201706 HR 1706]
- [http://webviz.u-strasbg.fr/viz-bin/VizieR-S?CCDM%20J05154%2b3242A CCDM J05154+3242]
- [http://aladin.u-strasbg.fr/AladinPreview?-c=05+15+24.3929%2B32+41+15.361&ident=V*+KW+Aur&submit=Aladin+previewer Image 14 Aurigae]
{{Stars of Auriga}}
{{DEFAULTSORT:14 Aurigae}}
Category:A-type main-sequence stars
Category:F-type main-sequence stars