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BW Vulpeculae

In this article, we are going to explore BW Vulpeculae and its impact in different contexts. From its origin to its current evolution, BW Vulpeculae has been a topic of interest and debate in various areas. We will analyze its importance in contemporary society, its relevance in the academic field and its influence on technological development. Additionally, we will examine how BW Vulpeculae has shaped people's opinions and attitudes over time and how it continues to be a reference point in today's world. Through this comprehensive analysis, we hope to shed light on BW Vulpeculae and provide a more complete view of its impact on everyday life.

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BW Vulpeculae

A light curve for BW Vulpeculae, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 20h 54m 22.39491s[2]
Declination +28° 31′ 19.1827″[2]
Apparent magnitude (V) 6.54[3] (6.44 – 6.68)[4]
Characteristics
Spectral type B2 IIIv[5]
U−B color index −0.147±0.011[6]
Variable type β Cep[7]
Astrometry
Radial velocity (Rv)−6.1±3.0[8] km/s
Proper motion (μ) RA: +0.437[2] mas/yr
Dec.: −4.981[2] mas/yr
Parallax (π)1.1494±0.0652 mas[2]
Distance2,800 ± 200 ly
(870 ± 50 pc)
Absolute magnitude (MV)−2.47[9]
Details
Mass6.8±0.1[10] or 11−14[11] M☉
Luminosity515.14[6] L☉
Surface gravity (log g)3.71[12] cgs
Temperature23,014+919
−883[12] K
Metallicity 0.07±0.12[12] dex
Rotational velocity (v sin i)24±6[3] km/s
Age3.4±2.5[10] Myr
Other designations
AAVSO 2050+28, BW Vul, BD+27° 3909, HD 199140, HIP 103191, HR 8007, SAO 89265[13]
Database references
SIMBADdata

BW Vulpeculae or BW Vul, is a variable star in the northern constellation of Vulpecula. It is near the lower limit of visibility to the naked eye with a typical apparent visual magnitude of 6.54.[3] Based on an annual parallax shift of 1.15 mas,[2] the distance to BW Vul is about 2,800 light years. It is moving closer to the Earth with a baseline heliocentric radial velocity of around −6 km/s.[8]

This is a B-type giant star with a stellar classification of B2 IIIv,[5] where the 'v' suffix indicates variability in spectral features. Various authors have printed mass estimates ranging from 11 to 14 times the mass of the Sun,[11] although Tetzlaff et al. (2011) gives a mass of just 6.8 M☉.[10] It is about 3.4[10] million years old and is spinning with a projected rotational velocity of 24 km/s.[3] The star is typically radiating 515[6] times the Sun's luminosity from its photosphere at an effective temperature of 23,014 K.[12]

The variability of this star was announced in 1937, at the 58th Meeting of the American Astronomical Society by Canadian astronomer, Robert Methven Petrie.[14] It is a Beta Cephei variable that ranges between magnitudes 6.44 and 6.68 over a period of 4.8 hours.[4] For unknown reasons, the periodicity of the star has undergone sudden changes, followed by long periods of stability.[15] BW Vul is one of the most extreme β Cephei stars in terms of variability of light and radial velocity.[3][16] This is hypothesized as being due to the star's relatively high metallicity, meaning the abundance of elements other than hydrogen and helium.[11] A distinctive feature of its radial velocity cycle is a unique "standstill" feature, which is caused by a shockwave generated by infall of material from a previous cycle.[16]

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e f 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.
  3. ^ a b c d e Stankov, A.; et al. (September 2003). "Abundances and radial velocity analysis of BW Vulpeculae". Astronomy and Astrophysics. 408 (3): 1077–1086. Bibcode:2003A&A...408.1077S. doi:10.1051/0004-6361:20031005.
  4. ^ a b Otero, Sebastian Alberto (21 November 2011). "BW Vulpeculae". AAVSO Website. American Association of Variable Star Observers. Retrieved 2 August 2015.
  5. ^ a b Lynds, C. R. (September 1959). "The light-variability of early B giants". Astrophysical Journal. 130: 577. Bibcode:1959ApJ...130..577L. doi:10.1086/146747.
  6. ^ a b c 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.
  7. ^ Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  8. ^ a b Gontcharov, G. A. (November 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.
  9. ^ Gontcharov, G. A. (November 2012). "Spatial distribution and kinematics of OB stars". Astronomy Letters. 38 (11): 694–706. arXiv:1606.09028. Bibcode:2012AstL...38..694G. doi:10.1134/S1063773712110035. S2CID 119108982.
  10. ^ a b c d Tetzlaff, N.; et al. (January 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.
  11. ^ a b c Fokin, A.; et al. (November 2004). "Hydrodynamic models for β Cephei variables. I. BW Vulpeculae revisited". Astronomy and Astrophysics. 426 (2): 687–693. Bibcode:2004A&A...426..687F. doi:10.1051/0004-6361:20040418.
  12. ^ a b c d Niemczura, E.; Daszyńska-Daszkiewicz, J. (April 2005). "Metallicities of the β Cephei stars from low-resolution ultraviolet spectra". Astronomy and Astrophysics. 433 (2): 659–669. arXiv:astro-ph/0410440. Bibcode:2005A&A...433..659N. doi:10.1051/0004-6361:20040396. S2CID 14295631.. Note: value taken from .
  13. ^ "BW Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved September 7, 2018.
  14. ^ Petrie, R. M. (1939). "A new Beta Canis Majoris-type star". Publications of the American Astronomical Society. 9: 53. Bibcode:1939PAAS....9Q..53P.
  15. ^ Odell, A. P. (August 2012). "Period variation in BW Vulpeculae redux". Astronomy & Astrophysics. 544: 4. arXiv:1205.5996. Bibcode:2012A&A...544A..28O. doi:10.1051/0004-6361/201219418. S2CID 119279687. A28.
  16. ^ a b Smith, Myron A.; et al. (December 2005). "Far-Ultraviolet and Optical Observations of BW Vulpeculae". The Astrophysical Journal. 634 (2): 1300–1310. Bibcode:2005ApJ...634.1300S. doi:10.1086/497026.
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