S Vulpeculae

S Vulpeculae

A visual band light curve for S Vulpeculae, adapted from Heiser (1996)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 19h 48m 23.8064s[2]
Declination 27° 17′ 11.4265″[2]
Apparent magnitude (V) 8.974[3] (8.69 - 9.42[4])
Characteristics
Spectral type G0-K2(M1)[5]
U−B color index +1.3 - +2.0[6]
B−V color index +1.7 - +2.1[6]
Variable type δ Cep[4]
Astrometry
Radial velocity (Rv)0.0 ± 2[7] km/s
Proper motion (μ) RA: −3.401±0.058[2] mas/yr
Dec.: −5.923±0.059[2] mas/yr
Parallax (π)0.3050 ± 0.0406 mas[2]
Distanceapprox. 11,000 ly
(approx. 3,300 pc)
Absolute magnitude (MV)−6.08[3]
Details[3]
Mass14.2 M☉
Radius382[8] R☉
Luminosity28,840 L☉
Temperature4,477 K
Metallicity [Fe/H]−0.01[9] dex
Age12.6 Myr
Other designations
S Vulpeculae, SAO 87743, HD 338867, BD+26°3674, AAVSO 1944+27
Database references
SIMBADdata

S Vulpeculae is a variable star located in the constellation Vulpecula. A supergiant star,[10] it is around 382 times the diameter of the Sun.[8]

S Vulpeculae was first suspected of varying in brightness in 1836 and this was confirmed by 1862. A pulsating variable that grows and shrinks as it changes in brightness, it has been variously classified as an RV Tauri variable, a semiregular variable star, or a Cepheid variable.[11][5]

S Vulpeculae is now confirmed as a classical Cepheid variable with one of the longest known periods at 68 days,[3] although the period has changed several times.[1] As such, it is also one of the cooler and more luminous of the Cepheids, and it lies close to the zone where semiregular variable stars are found. The shape and amplitude of the light curve varies significantly from cycle to cycle and secularly. The apparent magnitude ranges from 8.69 to 9.42.[4] The spectrum varies from early G to late K as it pulsates, with TiO bands typical of an M1 star when the star is coolest.[5]

  1. ^ a b Heiser, Arnold M. (1996). "BV Observations of the Long-Period Cepheid S Vulpeculae". Publications of the Astronomical Society of the Pacific. 108: 603. Bibcode:1996PASP..108..603H. doi:10.1086/133771.
  2. ^ a b c d e Cite error: The named reference Gaia DR2 was invoked but never defined (see the help page).
  3. ^ a b c d Turner, David G. (2014). "Towards a Determination of Definitive Parameters for the Long Period Cepheid S Vulpeculae". Odessa Astronomical Publications. 26: 115. arXiv:1403.1968. Bibcode:2013OAP....26..115T.
  4. ^ a b c 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.
  5. ^ a b c Joy, Alfred H. (1952). "The Semiregular Variable Stars of the RV Tauri and Related Classes". Astrophysical Journal. 115: 25. Bibcode:1952ApJ...115...25J. doi:10.1086/145506.
  6. ^ a b Berdnikov, L. N.; Ivanov, G. R. (1986). "On the Type of Variability of S Vul". Information Bulletin on Variable Stars. 2856: 1. Bibcode:1986IBVS.2856....1B.
  7. ^ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
  8. ^ a b Gieren, Wolfgang P.; Fouque, Pascal; Gomez, Matias (1998). "Cepheid Period‐Radius and Period‐Luminosity Relations and the Distance to the Large Magellanic Cloud". The Astrophysical Journal. 496 (1): 17–30. arXiv:astro-ph/9710161. Bibcode:1998ApJ...496...17G. doi:10.1086/305374. S2CID 14881794.
  9. ^ Marsakov, V. A.; Koval', V. V.; Kovtyukh, V. V.; Mishenina, T. V. (2013). "Properties of the population of classical Cepheids in the Galaxy". Astronomy Letters. 39 (12): 851. Bibcode:2013AstL...39..851M. doi:10.1134/S1063773713120050. S2CID 119788977.
  10. ^ Buscombe, W. (1974). "Supergiants in the Milky Way". Perem. Zvezdy. 2: 127. Bibcode:1974PZP.....2..127B.
  11. ^ Nassau, J. J.; Ashbrook, J. (1943). "S Vulpeculae". Astronomical Journal. 50: 97. Bibcode:1943AJ.....50...97N. doi:10.1086/105732.