Speaker
Description
In magnetic cataclysmic variables, X-ray emission is emitted from optically thin shock-heated plasma at the poles of the white dwarf. The X-ray emitting plasma has a continuous temperature distribution that can be reflected and/or reprocessing in the system before reaching the observer. The X-ray photons are reflected by the surface of the white dwarf, leading to a fluorescent iron K-alpha emission line at 6.4 keV and a Compton Hump in the 10-30 keV range, which leads to a harder spectrum. Furthermore, the pre-shock region and the surface of the WD can reprocess the X-ray emission, leading to a smooth hardening in soft X-rays. Both phenomena have substantial signatures in the X-ray spectrum, which must be taken into account to truly characterize the X-ray spectrum. The recent study of IGR J15094-4100 using the NuSTAR + XMM-Newton mission data shows that it has ionized and neutral material in absorption in the soft X-rays, as well as a harder spectrum due to the reflection effect. In this study, we present a detailed study of the X-ray spectrum of IGR J150194-4100 using eROSITA and NuSTAR data to characterize the X-ray spectrum and to reveal the phenomena contributing in the X-ray spectrum by comparing it with previous findings.
