Super Soft Sources
| dc.creator | Kahabka, P. | |
| dc.date | 2002-12-02 | |
| dc.date.accessioned | 2026-07-25T11:51:53Z | |
| dc.description | 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. | |
| dc.description | To appear in Compact Stellar X-Ray Sources, eds. W.H.G. Lewin and M. van der Klis, Cambridge University Press | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0212037 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0212037 | |
| dc.identifier.uri | https://dspace.dare.co.zw/handle/123456789/6301 | |
| dc.subject | Astrophysics | |
| dc.title | Super Soft Sources | |
| dc.type | text |