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W Cephei

Not to be confused with VV Cephei.
W Cephei

A visual band light curve for W Cephei, adapted from Polyakova (2006)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Cepheus
Right ascension 22h 36m 27.56307s[2]
Declination +58° 25′ 33.9554″[2]
Apparent magnitude (V) 6.83 - 9.20[3]
Characteristics
Evolutionary stage Red supergiant + non-supergiant B class star
Spectral type K0ep-M2ep Ia + B0/B1[3]
Variable type SRc[3]
Astrometry
Radial velocity (Rv)−44.64[4] km/s
Proper motion (μ) RA: −3.176[2] mas/yr
Dec.: −2.277[2] mas/yr
Distance2,427[5] pc
Absolute magnitude (MV)−7[6] + −3.5[7]
Orbit[8]
Period (P)2,075 d
Eccentricity (e)0.149
Inclination (i)90°
Details
Radius666.2+20.7
−11.1[2] R☉
Luminosity292,000[9] L☉
Surface gravity (log g)0.18[2] cgs
Temperature3,681[9] – 4,400[10] K
Metallicity0.0205[2]
Other designations
W Cep, BD+57°2568, HD 214369, HIP 111592, GSC 03995-00937, SAO 34614, PPM 40864, GC 31569, UCAC3 297-183471, IRAS 22345+5809, 2MASS J22362757+5825340, AAVSO 2232+57
Database references
SIMBADdata

W Cephei is a spectroscopic binary and variable star located in the constellation Cepheus. It is thought to be a member of the Cep OB1 stellar association at about 8,000 light years.[5][11] The supergiant primary star is one of the largest known stars and as well as one of the most luminous red supergiants.

  1. ^ Cite error: The named reference Polyakova was invoked but never defined (see the help page).
  2. ^ a b c d e f g 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 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.
  4. ^ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430 (1): 165. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
  5. ^ a b Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430 (1): 165. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
  6. ^ Cite error: The named reference wallerstein was invoked but never defined (see the help page).
  7. ^ Stickland, David J. (1988). "IUE and stars with composite spectra". In ESA. 281: 27. Bibcode:1988ESASP.281b..27S.
  8. ^ Petrova, A. V.; Orlov, V. V. (1999). "Apsidal Motion in Double Stars. I. Catalog". The Astronomical Journal. 117 (1): 587. Bibcode:1999AJ....117..587P. doi:10.1086/300671. S2CID 122386285.
  9. ^ a b Dorn-Wallenstein, Trevor Z.; Levesque, Emily M.; Neugent, Kathryn F.; Davenport, James R. A.; Morris, Brett M.; Gootkin, Keyan (2020). "Short Term Variability of Evolved Massive Stars with TESS II: A New Class of Cool, Pulsating Supergiants". The Astrophysical Journal. 902 (1): 24. arXiv:2008.11723. Bibcode:2020ApJ...902...24D. doi:10.3847/1538-4357/abb318. S2CID 221340538.
  10. ^ Garmany, C. D.; Stencel, R. E. (1992). "Galactic OB associations in the northern Milky Way Galaxy. I - Longitudes 55 deg to 150 deg". Astronomy and Astrophysics Supplement Series. 94: 211. Bibcode:1992A&AS...94..211G.
  11. ^ Cite error: The named reference polyakova was invoked but never defined (see the help page).

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