📝 SummarXiv

Abstract

About 12 percent of the early-type Be stars, so-called gamma Cas stars, exhibit an unusually hard and bright thermal X-ray emission that could result from accretion onto a white dwarf companion or from magnetic interactions between the Be star and its decretion disk. Exploring the full power of high-resolution X-ray spectroscopy of gamma Cas stars requires comparison of observations of the fluorescent Fe Kalpha emission lines near 6.4 keV with synthetic profiles of this line complex computed in the framework of the magnetic interaction and the accreting WD scenarios. For the latter, we further distinguish between accretion onto a non-magnetic and a magnetic WD. Our models account for different reservoirs of reprocessing material: the Be circumstellar decretion disk, the Be photosphere, an accretion disk around the WD companion, a magnetically channelled accretion flow and the WD photosphere. We find considerably different line properties for the different scenarios. For a non-magnetic accreting WD, the global Fe Kalpha complex is extremely broad, reaching a full width of 140 eV, whilst it is ~ 40 eV for the magnetic star-disk interaction and the magnetic accreting WD cases. In the magnetic star-disk interaction, the line centroid follows the orbital motion of the Be star, whereas it moves along with the WD in the case of an accreting WD. For gamma Cas, given the 15 times larger amplitude of the WD orbital motion, the shift in position for an accreting WD should be easily detectable with high-resolution spectrographs such as Resolve on XRISM, but remains essentially undetectable for the magnetic star-disk interaction. Upcoming high-resolution spectroscopy of the fluorescent Fe Kalpha emission lines in the X-ray spectra of gamma Cas stars will thus allow to distinguish between the competing scenarios.