Volume 615, July 2018
|Number of page(s)||19|
|Published online||10 July 2018|
Intriguing X-ray and optical variations of the γ Cassiopeiae analog HD 45314★
Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liége,
Allée du 6 Août, 19c, Bât B5c,
2 National Optical Astronomical Observatory, 950 N. Cherry Ave., Tucson, AZ, USA
3 Department of Physics and Astronomy, University of North Carolina at Greensboro, Greensboro, NC 27412, USA
4 Balmes, 2, 08784 Piera, Barcelona, Spain
5 Observatori Puig d’Agulles, Passatge Bosc 1, 08759 Vallirana, Barcelona, Spain
6 Kernersville Observatory, Kernersville, NC, USA
7 Hamburger Sternwarte, Universität Hamburg, Hamburg, Germany
8 Departamento de Astronomía, Universidad de Guanajuato, Guanajuato, Mexico
9 Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada 22800, Baja California, Mexico
Accepted: 25 January 2018
Context. A growing number of Be and Oe stars, named the γ Cas stars, are known for their unusually hard and intense X-ray emission. This emission could either trace accretion by a compact companion or magnetic interaction between the star and its decretion disk.
Aims. To test these scenarios, we carried out a detailed optical monitoring of HD 45314, the hottest member of the class of γ Cas stars, along with dedicated X-ray observations on specific dates.
Methods. High-resolution optical spectra were taken to monitor the emission lines formed in the disk, while X-ray spectroscopy was obtained at epochs when the optical spectrum of the Oe star was displaying peculiar properties.
Results. Over the last four years, HD 45314 has entered a phase of spectacular variations. The optical emission lines have undergone important morphology and intensity changes including transitions between single- and multiple-peaked emission lines as well as shell events, and phases of (partial) disk dissipation. Photometric variations are found to be anti-correlated with the equivalent width of the Hα emission. Whilst the star preserved its hard and bright X-ray emission during the shell phase, the X-ray spectrum during the phase of (partial) disk dissipation was significantly softer and weaker.
Conclusions. The observed behaviour of HD 45314 suggests a direct association between the level of X-ray emission and the amount of material simultaneously present in the Oe disk as expected in the magnetic star-disk interaction scenario.
Key words: stars: emission-line, Be / stars: individual: HD 45314 / X-rays: stars
© ESO 2018
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