Discovery of Rapidly Moving Partial X-Ray Absorbers Within Cassiopeiae

• Published in: Astrophysical journal. Letters Vol. 832; no. 2
• Main Authors: Hamaguchi, K., Oskinova, L., Russell, C. M. P., Petre, R., Enoto, T., Morihana, K., Ishida, M.
• Format: Journal Article
• Language: English
• Published: Goddard Space Flight Center The American Astronomical Society 23.11.2016
• Subjects: Astrophysics; Be Aeuro" Stars: Individual; Tars: Emission-Line
• ISSN: 2041-8213

Gamma Cassiopeiae is an enigmatic Be star with unusually strong hard X-ray emission. The Suzaku observatory detected six rapid X-ray spectral hardening events called "softness dips" in a approx.100 ks observation in 2011. All the softness dip events show symmetric softness-ratio variations, and some of them have flat bottoms apparently due to saturation. The softness dip spectra are best described by either approx.40% or approx.70% partial covering absorption to kT approx.12 keV plasma emission by matter with a neutral hydrogen column density of approx.(2−8) ×10(exp 21)/sq cm, while the spectrum outside these dips is almost free of absorption. This result suggests the presence of two distinct X-ray-emitting spots in the gamma Cas system, perhaps on a white dwarf (WD) companion with dipole mass accretion. The partial covering absorbers may be blobs in the Be stellar wind, the Be disk, or rotating around the WD companion. Weak correlations of the softness ratios to the hard X-ray flux suggest the presence of stable plasmas at kT approx 0.9 and 5 keV, which may originate from the Be or WD winds. The formation of a Be star and WD binary system requires mass transfer between two stars; gamma Cas may have experienced such activity in the past.