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BE Camelopardalis - Wikipedia

  • ️Mon Mar 01 2021

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BE Camelopardalis


A light curve for BE Camelopardalis, plotted from Hipparcos data[1]

Observation data
Epoch J2000      Equinox J2000
Constellation Camelopardalis
Right ascension 03h 49m 31.27755s[2]
Declination +65° 31′ 33.5258″[2]
Apparent magnitude (V) 4.39[3] (4.35 - 4.48)[4]
Characteristics
Evolutionary stage asymptotic giant branch[5]
Spectral type M2 II[6]
B−V color index 1.870±0.029[3]
Variable type Lc[4]
Astrometry
Radial velocity (Rv)−1.70±1.47[3] km/s
Proper motion (μ) RA: +0.319 mas/yr[2]
Dec.: −15.593 mas/yr[2]
Parallax (π)3.3288 ± 0.1874 mas[2]
Distance958+53
−51 ly
(293.7+16.4
−15.5 pc)[7]
Absolute magnitude (MV)−2.51[3]
Details
Mass2.93[8] M☉
Radius250[9] R☉
Luminosity10,600[9] L☉
Temperature3,660[9] K
Other designations

BE Cam, BD+65°369, HD 23475, HIP 17884, HR 1155, SAO 12916[10]

Database references
SIMBADdata

BE Camelopardalis is a solitary[11] variable star in the northern circumpolar constellation of Camelopardalis. It is visible to the naked eye as a faint, red-hued point of light with an apparent visual magnitude that fluctuates around 4.39.[3] The star is located roughly 960 light years away.[7]

This object is an M-type bright giant with a stellar classification of M2 II,[6] and is currently on the asymptotic giant branch. In 1928, Joel Stebbins and Charles Morse Huffer announced that the star, then called HR 1155, is a variable star, based on observations made at Washburn Observatory.[12] It was given its variable star designation, BE Camelopardalis, in 1977.[13] It is classified as an irregular variable of subtype Lc and its brightness varies from magnitude +4.35 down to +4.48.[4] Having exhausted the supply of hydrogen at its core, the star has expanded to around 250[9] times the Sun's radius. It has 2.9[8] times the Sun's mass and is radiating over 10,000 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,660 K.[9]

  1. ^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b c d e 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.
  4. ^ a b c Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  5. ^ Eggen, Olin J. (July 1992). "Asymptotic giant branch stars near the sun". Astronomical Journal. 104 (1): 275–313. Bibcode:1992AJ....104..275E. doi:10.1086/116239.
  6. ^ a b Levesque, Emily M.; et al. (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID 15109583.
  7. ^ a b Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021-03-01). "Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. ISSN 0004-6256. Data about this star can be seen here.
  8. ^ a b Hohle, M. M.; et al. (2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331 (4): 349. arXiv:1003.2335. Bibcode:2010AN....331..349H. doi:10.1002/asna.200911355. S2CID 111387483.
  9. ^ a b c d e Healy, Sarah; Horiuchi, Shunsaku; Molla, Marta Colomer; Milisavljevic, Dan; Tseng, Jeff; Bergin, Faith; Weil, Kathryn; Tanaka, Masaomi (2024-03-23). "Red Supergiant Candidates for Multimessenger Monitoring of the Next Galactic Supernova". Monthly Notices of the Royal Astronomical Society. 529 (4): 3630–3650. arXiv:2307.08785. Bibcode:2024MNRAS.529.3630H. doi:10.1093/mnras/stae738. ISSN 0035-8711.
  10. ^ "BE Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-12.
  11. ^ 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.
  12. ^ Stebbins, Joel; Huffer, C. M. (1928). "The Constancy of the Light of Red Stars". Publications of the Washburn Observatory. 15: 137–174. Bibcode:1928PWasO..15..137S. Retrieved 5 December 2024.
  13. ^ Kukarkin, B. V.; Kholopov, P. N.; Fedorovich, V. P.; Kireyeva, N. N.; Kukarkina, N. P.; Medvedeva, G. I.; Perova, N. B. (March 1977). "62nd Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 1248: 1. Bibcode:1977IBVS.1248....1K. Retrieved 29 December 2024.