Astronomy:54 Aurigae

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Short description: Multiple star system in the constellation Auriga
54 Aurigae
54AurLightCurve.png
A light curve for 54 Aurigae, plotted from TESS data[1]
Observation data
{{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}}
Constellation Auriga
A
Right ascension  06h 39m 33.12003s[2]
Declination +28° 15′ 47.2764″[2]
Apparent magnitude (V) 6.22[3]
B
Right ascension  06h 39m 33.11965s[2]
Declination +28° 15′ 47.2740″[2]
Apparent magnitude (V) 7.82[3]
Characteristics
Spectral type B7 III[4]
B−V color index −0.087±0.007[5]
Variable type Algol[6]
Astrometry
A
Radial velocity (Rv)+19.0±4.3[5] km/s
Proper motion (μ) RA: −5.461[2] mas/yr
Dec.: −10.523[2] mas/yr
Parallax (π)3.5961 ± 0.0952[2] mas
Distance910 ± 20 ly
(278 ± 7 pc)
Details
54 Aur A
Luminosity315.49[7] L☉
Temperature11,083[7] K
Rotational velocity (v sin i)65[8] km/s
Other designations
54 Aur, NSV 3065, BD+28°1196, FK5 2504, GC 8681, HD 47395, HIP 31852, HR 2438, SAO 78593, ADS 5289, WDS J06395+2816[9]
Database references
SIMBADdata

54 Aurigae is a multiple star system located around 800 light-years (51,000,000 AU) away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, blue-white hued star with a combined apparent visual magnitude of 6.02.[5] The system is moving further from the Sun with a heliocentric radial velocity of around +19 km/s.[5]

54 Aurigae is resolved into two visible components, of magnitudes 6.22 and 7.82, separated by 0.8″. The double was discovered in 1843 when the separation was only 0.7″.[10] There is no separate measure of the parallax of the secondary, but it shares a common proper motion with the brighter star[11] and they are assumed to form a binary.[10] The spectral class B7 III is assigned to the brighter of the pair, indicating a hot giant star, although it has also been given as B7/8 III/V, suggesting it may be a main sequence star.[12] Most sources can't give a separate spectral classification for the fainter star, but it has been listed as DA1/K4V, indicating it is either a white dwarf or red dwarf.[13]

The brighter component of the visible pair is an eclipsing binary with a period of 1.8797 days, and a primary eclipse depth of 0.03 magnitudes.[14] It is radiating 315 times the luminosity of the Sun from its photosphere at an effective temperature of 11,083 K (10,810 °C; 19,490 °F),[7] and is spinning with a projected rotational velocity of 65 kilometres per second (40 mi/s).[8]

References

  1. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 7 October 2022. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  4. ↑ Cucchiaro, A. et al. (October 1977), "Spectral classification from the ultraviolet line features of S2/68 spectra. II - Late B-type stars", Astronomy and Astrophysics Supplement Series 30: 71–79, Bibcode: 1977A&AS...30...71C. 
  5. ↑ 5.0 5.1 5.2 5.3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  6. ↑ NSV 3065, AAVSO, https://www.aavso.org/vsx/index.php?view=detail.top&oid=41689, retrieved 7 October 2022. 
  7. ↑ 7.0 7.1 7.2 McDonald, I. et al. (2012), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society 427 (1): 343–357, doi:10.1111/j.1365-2966.2012.21873.x, Bibcode: 2012MNRAS.427..343M. 
  8. ↑ 8.0 8.1 Abt, Helmut A. et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A 
  9. ↑ "54 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=54+Aur. 
  10. ↑ 10.0 10.1 Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (December 2001), "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog", The Astronomical Journal 122 (6): 3466–3471, doi:10.1086/323920, ISSN 0004-6256, Bibcode: 2001AJ....122.3466M. 
  11. ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  12. ↑ Clausen, J. V.; Jensen, K. S. (1979), "Classification Based on 102/A/Mm Objective Prism Spectra", IAU Colloq. 47: Spectral Classification of the Future 9: 479, Bibcode: 1979RA......9..479C. 
  13. ↑ Pickles, A.; Depagne, É. (2010), "All-Sky Spectrally Matched UBVRI - ZY and u′ g′ r′ i′ z′ Magnitudes for Stars in the Tycho2 Catalog", Publications of the Astronomical Society of the Pacific 122 (898): 1437, doi:10.1086/657947, Bibcode: 2010PASP..122.1437P. 
  14. ↑ Wraight, K. T.; White, Glenn J.; Bewsher, D.; Norton, A. J. (October 2011), "STEREO observations of stars and the search for exoplanets", Monthly Notices of the Royal Astronomical Society 416 (4): 2477–2493, doi:10.1111/j.1365-2966.2011.18599.x, Bibcode: 2011MNRAS.416.2477W. 



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