14 Aurigae
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 15m 24.39398s[1] |
Declination | +32° 41′ 15.3638″[1] |
Apparent magnitude (V) | 5.01[2] (5.08 + 7.86)[3] |
Characteristics | |
Spectral type | A9IV + ? + F5V + M3V: + WDA[3] |
U−B color index | +0.19[4] |
B−V color index | +0.222±0.004[2] |
Variable type | δ Scuti[5] |
Astrometry | |
Radial velocity (Rv) | −9.3±0.2[2] km/s |
Proper motion (μ) | RA: −25.062[1] mas/yr Dec.: +12.056[1] mas/yr |
Parallax (π) | 12.1306 ± 0.1712 mas[1] |
Distance | 269 ± 4 ly (82 ± 1 pc) |
Absolute magnitude (MV) | 0.31[2] |
Details | |
14 Aur Aa | |
Mass | 1.64[6] M☉ |
Luminosity | 62.07[2] L☉ |
Surface gravity (log g) | 3.46[7] cgs |
Temperature | 7,498[7] K |
Metallicity [Fe/H] | −0.02[2] dex |
Rotation | 2.11 h[5] |
Rotational velocity (v sin i) | 27.6[7] km/s |
Age | 609[6] Myr |
Other designations | |
Database references | |
SIMBAD | data |
14 Aurigae is a quintuple star system located 269[1] 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.[8] It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.01.[2] The system is moving closer to the Sun with a heliocentric radial velocity of −9 km/s.[2]
The magnitude 5.08[3] primary member, designated component A, is a single-lined spectroscopic binary system in a circular orbit with a period of 3.7887 days.[9] The visible member has a stellar classification of A9 IV or A V, depending on the source,[10] and is a Delta Scuti variable with an amplitude of 0.08 magnitude and a period of 2.11 hours.[5] It is 609 million years old with 1.64 times the mass of the Sun.[6]
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,[3] 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.[10]
References
- ^ 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
{{citation}}
: CS1 maint: unflagged free DOI (link) - ^ 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.; et al. (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. Bibcode:2009A&A...493.1099S. doi:10.1051/0004-6361:200810377.
- ^ 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.
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: CS1 maint: unflagged free DOI (link)