Supersoft X-ray sources in the magellanic clouds

Details Supersoft X-ray sources in the magellanic clouds Supersoft X-ray sources in the magellanic clouds

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995adspr..16..149k&link_type=abstract

Advances in Space Research (ISSN 0273-1177), vol. 16, no. 3, p. 149-153

Astronomy and Astrophysics

Astronomy

All Sky Photography, Magellanic Clouds, Mapping, Rosat Mission, X Ray Astronomy, X Ray Sources, Accretion Disks, Black Body Radiation, Mass Flow, Planetary Nebulae, Stellar Evolution

Scientific paper

The Magellanic Clouds (MCs) have been mapped at soft X-rays (0.1-2.4 keV) with ROSAT during an all-sky survey and numerous pointed observations. A distinct class of supersoft X-ray sources (SSS) was discovered radiating with blackbody temperatures of a few times 105 K and with bolometric luminosities approximately 104 times solar. A detailed study of these sources in X-rays, UV and the optical spectral regime has just started. The nature of these sources was in debate with a black hole (Cowley et al. 1990), neutron star (Kylafis & Xilouris 1993) and white dwarf (Van den Heuvel et al. 1992) origin. The identification of SSS in the Small Magellanic Cloud with the hot central star of a planetary nebula (Wang 1991) and the hot component of a symbiotic nova (Kahabka et al. 1994) are in favor for a white dwarf (WD) origin. Van den Heuvel et al. 1992 have shown, that Cal 83 and Cal 87 in the Large Magellanic Cloud are close binaries with a WD accreting at high rates and stable burning hydrogen. Systems of a similar nature may be RXJ0513.9-6951 and 1E0035.4-7230. SSS are observed to be stable burning already for a period of approximately 10 years or are of transient nature or even recurrent. Such a behavior is predicted for accreting and nuclear burning WDs if the accretion rate is within or below a critical range (Fujimoto 1982).

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