Luminous Supersoft X-ray sources: RXJ0527, RXJ0513.9-6951, RXJ0537 and XMMUJ0520
Abstract
A steady state model has been considered to explain the observed characteristics of luminous supersoft X- ray sources RXJO527, RXJ0513.9-6951, RXJ0537 and XMMUJ0520. The model is of an accreting white dwarf (WD) in a close binary with a main-sequence star, subgiant, or giant. When accretion rate is (∼ 1× 10^{-7} M_{⊙} yr^{-1} - 5× 10^{-7}M_{⊙} yr^{-1}) hydrogen shell burning consumes hydrogen at the same rate as the white dwarf accretes it. The accreting matter containing small fraction of C, O, Ne, Mg will capture proton at high temperature and density condition leading to CNOF, NeNa, MgALSi cyclic reactions. Using most recent proton capturing reaction rates and beta-decay rates the cyclic reactions have been studied and examined about the energy generation during supersoft X-ray outburst time scale. The presently calculated values of effective temperature, luminosity etc tally well with the values observed by ROSAT and XMM-Newton observatories. Absorptive and electron-scattering opacities at layers of the envelope and color temperature near the photosphere have been determined. In the present work, possible absorption lines have been calculated and compared with the observed one.
- Publication:
-
The X-ray Universe 2014
- Pub Date:
- July 2014
- Bibcode:
- 2014xru..confE..35B