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Gamma Cassiopeiae variable

"GCAS" redirects here. For the privately funded graduate school, see Global Center for Advanced Studies.

A Gamma Cassiopeiae variable (γ Cassiopeiae variable) is a type of variable star, named for its prototype γ Cassiopeiae.

Variability

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A light curve for Gamma Cassiopeiae, plotted from data published by Labadie-Bartz et al. (2021)[1]

γ Cassiopeiae variables show irregular changes in brightness on a timescale of decades. These typically have amplitudes of the order of a magnitude. For example, γ Cassiopeiae is usually about magnitude 2.5 and has varied between magnitudes 1.6 and 3.0. The variations are associated with changes in the spectrum between normal absorption spectra and Be star spectra, often also including shell star characteristics.[2]

Pleione and γ Cassiopeiae itself are both variable stars that have intermittent shell episodes where strong shell features appear in the spectrum and the brightness increases or decreases significantly. At other times the shell is not detectable in the spectrum, and even the emission lines may disappear.[3]

The General Catalogue of Variable Stars (GCVS) categorises γ Cassiopeiae stars as eruptive variables and describes them as rapidly-rotating B class giants or subgiants, although many of them are main sequence stars. It distinguishes them from those Be stars that only show smaller amplitude brightness variations. The GCVS uses the code GCAS to denote γ Cassiopeiae variables.[2]

Mechanism

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γ Cassiopeiae variables are understood to be hot stars which have equatorial decretion disks which periodically disappear and reform, or possibly just change dramatically in scale. They are probably all very rapid rotators and most can be classified as Be stars. They are often also shell stars at least part of the time, where the disk is seen edge-on and produces very narrow absorption lines in addition to the broader photospheric lines and possible emission lines. Regardless of whether they are shell stars by the most narrow definition, the periods when they produce strong disks and increase in brightness are known as shell events.[3]

Examples

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Designation (name) Constellation Discovery Apparent magnitude (Maximum)[A] Apparent magnitude (Minimum)[A] Range of magnitude Period Spectral class Comment
Gamma Cassiopeiae Cassiopeia   1m.6 3m.0 1.4 B0.5 IVe Prototype
Delta Scorpii A[4] Scorpius 1m.59 2m.32 0.73 B0.3 IV[5]
Kappa Canis Majoris Canis Major   3m.40 3m.97 0.57 B1.5IVne  
Beta Canis Minoris Canis Minor 2m.84[6] 2m.92[6] 0.08 B8V e[7]
FW Canis Majoris Canis Major   5m.00 5m.50 0.50  
Zeta Ophiuchi Ophiuchus 2m.56[8] 2m.58[8] 0.02 O9.5V[9] Also a Beta Cephei variable
Pleione Taurus 4m.77[6] 5m.5[6] 0.77 B8Vne[10]
Lambda Pavonis Pavo   4m.00 4m.26 0.26 B2II-IIIe  
Phi Persei[11] Perseus   3m.96 4m.11 0.15 19.5 d B2Vpe  
Psi Persei[11] Perseus   4m.17 4m.36 0.19 B5III-Vne  
X Persei Perseus   6m.03 7m.0 0.97 B0Ve Also a High-mass X-ray binary
A (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))

References

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  1. ^ Labadie-Bartz, Jonathan; Baade, Dietrich; Carciofi, Alex C.; Rubio, Amanda; Rivinius, Thomas; Borre, Camilla C.; Martayan, Christophe; Siverd, Robert J. (March 2021). "Short-term variability and mass loss in Be stars – VI. Frequency groups in γ Cas detected by TESS". Monthly Notices of the Royal Astronomical Society. 502 (1): 242–259. arXiv:2012.06454. doi:10.1093/mnras/staa3913. Retrieved 23 July 2022.
  2. ^ a b 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: B/gcvs. Bibcode:2009yCat....102025S.
  3. ^ a b Rivinius, Thomas; Carciofi, Alex C.; Martayan, Christophe (2013). "Classical be stars. Rapidly rotating B stars with viscous Keplerian decretion disks". Astronomy and Astrophysics Review. 21: 69. arXiv:1310.3962. Bibcode:2013A&ARv..21...69R. doi:10.1007/s00159-013-0069-0. S2CID 118652497.
  4. ^ "VSX : Detail for del Sco". www.aavso.org. Retrieved 2023-12-18.
  5. ^ Balona, L. A.; Dziembowski, W. A. (1999-10-01). "Excitation and visibility of high-degree modes in stars". Monthly Notices of the Royal Astronomical Society. 309 (1): 221–232. Bibcode:1999MNRAS.309..221B. doi:10.1046/j.1365-8711.1999.02821.x. ISSN 0035-8711.
  6. ^ a b c d Samus, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2009-01-01). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+, 2007-2017)". VizieR Online Data Catalog: B/gcvs. Bibcode:2009yCat....102025S.
  7. ^ Saio, H.; Cameron, C.; Kuschnig, R.; Walker, G. a. H.; Matthews, J. M.; Rowe, J. F.; Lee, U.; Huber, D.; Weiss, W. W. (2006-09-16). "MOST Detects g -Modes in the Late-Type be Star β Canis Minoris (B8 Ve)". The Astrophysical Journal. 654: 544–550. arXiv:astro-ph/0609460. doi:10.1086/509315.
  8. ^ a b Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017-01-01). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. ISSN 1063-7729.
  9. ^ Hubrig, S.; Oskinova, L. M.; Schoeller, M. (2011-01-28). "First detection of a magnetic field in the fast rotating runaway Oe star ζ Ophiuchi". Astronomische Nachrichten. 332 (2): 147–152. arXiv:1101.5500v1. Bibcode:2011AN....332..147H. doi:10.1002/asna.201111516.
  10. ^ Taranova, O.; Shenavrin, V.; Nadjip, A. D. (2008-02-01). "Pleione (BU Tau): IR Fading of the Star in 1999 - 2007". Peremennye Zvezdy Prilozhenie. 8 (6): 6. Bibcode:2008PZP.....8....6T. ISSN 0373-7683.
  11. ^ a b Tur, N. S.; Goraya, P. S. (April 1988). "Scanner observations of shell stars Phi Persei and Psi Persei". Astrophysics and Space Science. 143 (1): 99–105. Bibcode:1988Ap&SS.143...99T. doi:10.1007/BF00636758. S2CID 121741933.

Further reading

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