V381 Cephei

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V381 Cephei
Cepheus constellation map.svg
Red circle.svg
Location of V381 Cephei (circled)
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Cepheus
Right ascension 21h 19m 15.682s [1]
Declination +58° 37′ 24.550″ [1]
Apparent magnitude  (V)5.51 - 5.71 [2]
Characteristics
Spectral type M1epIb + B [3]
U−B color index 0.00 [4]
B−V color index +1.34 [4]
Variable type Lc [2]
Astrometry
Radial velocity (Rv)−14.10 [5]  km/s
Proper motion (μ)RA: −1.435 [6]   mas/yr
Dec.: −5.427 [6]   mas/yr
Parallax (π)1.59 ± 0.23  mas [6]
Distance approx. 2,100  ly
(approx. 630  pc)
Absolute magnitude  (MV)−5.2 [7]
Details
Aa
Mass 7.2 [8] - 16 [9]   M☉
Radius 977 [10]   R☉
Luminosity 178,000 [10]   L☉
Temperature 3,745±170 [1] [10]   K
Ab
Mass 13 [9]   M☉
B
Mass 7.1 [11]   M☉
Radius 3.4 [12]   R☉
Luminosity 1,487 [12]   L☉
Surface gravity (log g)4.18 [12]   cgs
Temperature 19,965 [12]   K
Metallicity [Fe/H]−0.30 [11]   dex
Rotational velocity (v sin i)42.8 [13]  km/s
Age 49.1 [8]   Myr
Other designations
V381  Cephei, HR  8164, HIP  105259, BD+58°2249, ADS  14864, 2MASS  J21191567+5837246, WDS  J21193+5837
A: HD  203338
B: HD  203339
Database references
A
B

V381 Cephei (HR 8164) is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.

Contents

System

V381 Cephei is a visual double star with components A and B separated by 4.6". The primary is HD 203338 and the secondary is the magnitude 9.2 HD 203339. [9]

HD 203338 is itself a spectroscopic binary with components Aa and Ab orbiting every 280 years. [9] It forms a VV Cephei-type binary system with a hot companion which is accreting mass from the primary. The long period means that it exhibits fewer peculiarities than other VV Cephei binaries. [14]

Properties

A visual band light curve for V381 Cephei, adapted from Halbedel (1991) V381CepLightCurve.png
A visual band light curve for V381 Cephei, adapted from Halbedel (1991)

Component Aa is a red supergiant and its close companion is a B2 main sequence star. The supergiant is a pulsating variable with a small amplitude and poorly defined period. It is generally given spectral class qualifiers indicating peculiarities and emission, which may be associated with the disc around the hot secondary. [14]

Component B, HD 203339, is a B3 main sequence star with a mass around 11  M☉. [9]

Related Research Articles

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References

  1. 1 2 3 Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal. 158 (1): 20. arXiv: 1905.03744 . Bibcode:2019AJ....158...20M. doi: 10.3847/1538-3881/ab1cbd . S2CID   148571616.
  2. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. ↑ Josselin, E.; Plez, B. (2007). "Atmospheric dynamics and the mass loss process in red supergiant stars". Astronomy and Astrophysics. 469 (2): 671. arXiv: 0705.0266 . Bibcode:2007A&A...469..671J. doi:10.1051/0004-6361:20066353. S2CID   17789027.
  4. 1 2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  5. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  6. 1 2 3 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.
  7. ↑ Stothers, R.; Leung, K. C. (1971). "Luminosities, masses and periodicities of massive red supergiants". Astronomy and Astrophysics. 10: 290. Bibcode:1971A&A....10..290S.
  8. 1 2 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID   118629873.
  9. 1 2 3 4 5 Tokovinin, A. A. (1997). "MSC - a catalogue of physical multiple stars". Astronomy and Astrophysics Supplement Series. 124: 75–84. Bibcode:1997A&AS..124...75T. doi: 10.1051/aas:1997181 .
  10. 1 2 3 Healy, Sarah; Horiuchu, Shunsaku; Colomer Moller, Marta; Milisavljevic, Dan; Tseng, Jeff; Bergin, Faith; Weil, Kathryn; Tanaka, Masaomi (17 July 2023). "Red Supergiant Candidates for Multimessenger Monitoring of the Next Galactic Supernova". arXiv: 2307.08785 .
  11. 1 2 Anders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardevol, J.; Casamiquela, L.; Figueras, F.; Jimenez-Arranz, O.; Jordi, C.; Monguio, M.; Romero-Gomez, M.; Altamirano, D.; Antoja, T.; Assaad, R.; Cantat-Gaudin, T.; Castro-Ginard, A.; Enke, H.; Girardi, L.; Guiglion, G.; Khan, S.; Luri, X.; Miglio, A.; Minchev, I.; Ramos, P.; Santiago, B. X.; Steinmetz, M. (2022). "VizieR Online Data Catalog: StarHorse2, Gaia EDR3 photo-astrometric distances (Anders+, 2022)". Vizier Online Data Catalog. Bibcode:2022yCat.1354....0A.
  12. 1 2 3 4 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.
  13. ↑ Glebocki, R.; Gnacinski, P. (2005). "VizieR Online Data Catalog: Catalog of Stellar Rotational Velocities (Glebocki+ 2005)". VizieR On-line Data Catalog: III/244. Originally Published in: 2005csss...13..571G; 2005yCat.3244....0G. 3244. Bibcode:2005yCat.3244....0G.
  14. 1 2 Halbedel, Elaine M. (1991). "Photometric variability for the VV Cephei-like star HR 8164". Astronomical Society of the Pacific. 103: 310. Bibcode:1991PASP..103..310H. doi: 10.1086/132820 . S2CID   120879494.
  15. ↑ Halbedel, Elaine M. (March 1991). "Photometric Variability for the VV Cephei-Like Star HR 8164". Publications of the Astronomical Society of the Pacific. 103: 310. Bibcode:1991PASP..103..310H. doi: 10.1086/132820 . S2CID   120879494.
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