astro.wikisort.org - Star

Search / Calendar

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

A light curve for 54 Aurigae, plotted from TESS data[1]
Observation data
Epoch J2000      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 mas[2]
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 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, retrieved 7 October 2022.
  2. Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
  3. 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.
  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. 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.
  6. "NSV 3065", The International Variable Star Index, AAVSO, retrieved 7 October 2022.
  7. McDonald, I.; et al. (2012), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–357, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  8. Abt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590
  9. "54 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-24.
  10. 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, Bibcode:2001AJ....122.3466M, doi:10.1086/323920, ISSN 0004-6256.
  11. 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.
  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, arXiv:1011.2020, Bibcode:2010PASP..122.1437P, doi:10.1086/657947, S2CID 54678796.
  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, Bibcode:2011MNRAS.416.2477W, doi:10.1111/j.1365-2966.2011.18599.x.

На других языках

- [en] 54 Aurigae

[ru] 54 Возничего

54 Возничего (лат. 54 Aurigae, HD 47395) — двойная звезда в созвездии Возничего на расстоянии (вычисленном из значения параллакса) приблизительно 843 световых лет (около 258 парсеков) от Солнца. Видимая звёздная величина звезды — +6,224m[2].


Текст в блоке "Читать" взят с сайта "Википедия" и доступен по лицензии Creative Commons Attribution-ShareAlike; в отдельных случаях могут действовать дополнительные условия.

Другой контент может иметь иную лицензию. Перед использованием материалов сайта WikiSort.org внимательно изучите правила лицензирования конкретных элементов наполнения сайта.

2019-2025
WikiSort.org - проект по пересортировке и дополнению контента Википедии