Super Soft Sources
Abstract
The class of Super Soft Sources has been established after discoveries performed with the Einstein and the ROSAT satellite. Only sources contributing to the class of super-soft X-ray binaries are considered. The X-ray emission in these sources is due to thermonuclear burning of accreted material on the surface of a white dwarf. The physical process of nuclear burning is described. The typical timescales of variability in these sources are discussed. The appearance and modeling of supersoft X-ray spectra are described. The phenomena related to the accretion disk in these sources are outlined. A discussion of the nature and appearance of the donor star is given. The evolutionary state of these sources and their likely progenitorship for Type Ia supernovae is shortly outlined. A summary of recent discoveries with Chandra and XMM-Newton of super-soft sources in nearby spiral and elliptical galaxies is given.
Cite
@article{arxiv.astro-ph/0212037,
title = {Super Soft Sources},
author = {P. Kahabka},
journal= {arXiv preprint arXiv:astro-ph/0212037},
year = {2007}
}
Comments
To appear in Compact Stellar X-Ray Sources, eds. W.H.G. Lewin and M. van der Klis, Cambridge University Press