Astronomy:W Virginis

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Short description: Variable star in the constellation Virgo
W Virginis
WVirLightCurve.png
A visual band light curve for W Virginis, adapted from Plachy et al. (2017)[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Virgo
Right ascension  13h 26m 01.9928s[2]
Declination −03° 22′ 43.4299″[2]
Apparent magnitude (V) 9.46[3] (9.46 - 10.75[4])
Characteristics
Spectral type F0Ib-G0Ib[4]
B−V color index +0.40[5] (+0.43 - +0.99[6])
Variable type W Virginis[4]
Astrometry
Radial velocity (Rv)−65.5[7] km/s
Proper motion (μ) RA: −3.944±0.094[2] mas/yr
Dec.: 1.027±0.102[2] mas/yr
Parallax (π)0.3986 ± 0.0663[2] mas
Distanceapprox. 8,000 ly
(approx. 2,500 pc)
Absolute magnitude (MV)−3.0[8]
Details
Mass0.4[9] M☉
Radius35[8] (22 - 52[6]) R☉
Luminosity851[9] (474 - 1,247[6]) L☉
Surface gravity (log g)0.0[10] cgs
Temperature4,280 - 6,550[6] K
Metallicity−1.0[10]
Other designations
HIP 65531, SAO 139335, BD-02° 3683, HD 116802[11]
Database references
SIMBADdata

W Virginis is the prototype W Virginis variable, a subclass of the Cepheid variable stars. It is located in the constellation Virgo, and varies between magnitudes 9.46 and 10.75 over a period of approximately 17 days.[4]

There are variations in the light curve apparently due to multiple pulsation periods rather than inherent instabilities in the pulsation. The dominant pulsation mode has a period of 17.27134 days with a period decrease detected over a 75-year period.[12]

The pulsations cause changes in both temperature and size, leading to large changes in the luminosity and brightness. The maximum temperature occurs when the star is at its brightest visually, when the star is also at its smallest. The minimum temperature and maximum radius occur at around phase 0.5 when the brightness is decreasing and nearly at minimum. Because relatively more infrared radiation is produced when the star is cooler, the maximum brightness in the infrared occurs when the visual brightness is already decreasing, and the maximum bolometric luminosity occurs at around phase 0.25 around halfway from maximum to minimum visual brightness.[6]

W Virginis stars are old helium shell burning stars with masses less than the sun. They have supergiant spectral luminosity classes despite their modest masses and actual luminosities, because they are highly inflated evolved stars with very low surface gravities. W Virginis itself is typical, with a mass less than half the sun, pulsating between 20 and 50 times the sun's radius, and a luminosity that varies from less than 500 L☉ to over a thousand L☉.

References

  1. ↑ Plachy, E.; Molnár, L.; Jurkovic, M. I.; Smolec, R.; Moskalik, P. A.; Pál, A.; Szabados, L.; Szabó, R. (February 2017). "First observations of W Virginis stars with K2: detection of period doubling". Monthly Notices of the Royal Astronomical Society 465 (1): 173–179. doi:10.1093/mnras/stw2703. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  3. ↑ 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: 0. Bibcode: 2002yCat.2237....0D. 
  4. ↑ 4.0 4.1 4.2 4.3 Samus, N. N. 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: 02025. Bibcode: 2009yCat....102025S. 
  5. ↑ Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Barker, Timothy; Baumgart, Leona D.; Butler, Dennis; Cudworth, Kyle M.; Kemper, Edward; Kraft, Robert P.; Lorre, Jean; Kameswara Rao, N. et al. (1971). "Abundance Analysis of Population II Variable Stars. I. W Virginis". Astrophysical Journal 165: 67. doi:10.1086/150877. Bibcode: 1971ApJ...165...67B. 
  7. ↑ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington: 0. Bibcode: 1953GCRV..C......0W. 
  8. ↑ 8.0 8.1 Balog, Z.; Vinko, J.; Kaszas, G. (1997). "Baade-Wesselink Radius Determination of Type II Cepheids". Astronomical Journal 113: 1833. doi:10.1086/118394. Bibcode: 1997AJ....113.1833B. 
  9. ↑ 9.0 9.1 Böhm-Vitense, E.; Szkody, P.; Wallerstein, G.; Iben, I. (1974). "Masses and luminosities of population II cepheids". Astrophysical Journal 194: 125. doi:10.1086/153229. Bibcode: 1974ApJ...194..125B. 
  10. ↑ 10.0 10.1 Maas, Thomas; Giridhar, Sunetra; Lambert, David L. (2007). "The Chemical Compositions of the Type II Cepheids-The BL Herculis and W Virginis Variables". The Astrophysical Journal 666 (1): 378–392. doi:10.1086/520081. Bibcode: 2007ApJ...666..378M. 
  11. ↑ "V* W Vir". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+W+Vir. 
  12. ↑ Templeton, M. R.; Henden, A. A. (2007). "Multicolor Photometry of the Type II Cepheid Prototype W Virginis". The Astronomical Journal 174 (5): 1999–2005. doi:10.1086/522945. Bibcode: 2007AJ....134.1999T. 



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