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  Short-term variability and mass loss in Be stars - V. Space photometry and ground-based spectroscopy of γ Cas

Borre, C. C., Baade, D., Pigulski, A., Panoglou, D., Weiss, A., Rivinius, T., et al. (2020). Short-term variability and mass loss in Be stars - V. Space photometry and ground-based spectroscopy of γ Cas. Astronomy and Astrophysics, 635: A140. doi:10.1051/0004-6361/201937062.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-8701-0 Version Permalink: http://hdl.handle.net/21.11116/0000-0006-8702-F
Genre: Journal Article

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 Creators:
Borre, C. C., Author
Baade, D., Author
Pigulski, A., Author
Panoglou, D., Author
Weiss, A.1, Author              
Rivinius, Th., Author
Handler, G., Author
Moffat, A. F. J., Author
Popowicz, A., Author
Wade, G. A., Author
Weiss, W. W., Author
Zwintz, K., Author
Affiliations:
1Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159882              

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 Abstract: Context. Be stars are physically complex systems that continue to challenge theory to understand their rapid rotation, complex variability, and decretion disks. γ Cassiopeiae (γ Cas) is one such star but is even more curious because of its unexplained hard thermal X-ray emission. Aims. We aim to examine the optical variability of γ Cas and thereby to shed more light on its puzzling behaviour. Methods. We analysed 321 archival Hα spectra from 2006 to 2017 to search for frequencies corresponding to the 203.5 day orbit of the companion. Space photometry from the SMEI satellite from 2003 to 2011 and the BRITE-Constellation of nano-satellites from 2015 to 2019 were investigated in the period range from a couple of hours to a few days. Results. The orbital period of the companion of 203.5 days is confirmed with independent measurements from the structure of the Hα line emission. A strong blue versus red asymmetry in the amplitude distribution across the Hα emission line could hint at a spiral structure in the decretion disk. With the space photometry, the known frequency of 0.82 d−1 is confirmed in data from the early 2000s. A higher frequency of 2.48 d−1 is present in the data from 2015 to 2019 and possibly in the early 2000s as well. A third frequency at 1.25 d−1 is proposed to exist in both SMEI and BRITE data. Seemingly, only a non-radial pulsation interpretation can explain all three variations. The two higher frequencies are incompatible with rotation.

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Language(s): eng - English
 Dates: 2020-03-23
 Publication Status: Published online
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 Identifiers: DOI: 10.1051/0004-6361/201937062
Other: LOCALID: 3237069
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Title: Astronomy and Astrophysics
  Other : Astron. Astrophys.
Source Genre: Journal
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Publ. Info: France : EDP Sciences S A
Pages: - Volume / Issue: 635 Sequence Number: A140 Start / End Page: - Identifier: ISSN: 1432-0746
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1