XMM-Newton Proposal 02012002

Details XMM-Newton Proposal 02012002 XMM-Newton Proposal 02012002

Mar 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003xmm..prop...65m&link_type=abstract

XMM-Newton Proposal ID #02012002

Computer Science

Hd 161103, Sao 49725, Xmm-Newton Proposal 02012002

Scientific paper

ROSAT observations have shown that the Be stars HD 161103 and SAO 49725 exhibit an excess of X-ray emission over the normal shocked wind component. The relatively modest X-ray luminosity of about 1 to 5 E32 erg/s (0.2-2.4 keV) is consistent with that expected from a white dwarf accreting from the equatorial disc of a Be star. Whereas models predict that they should outnumber Be + neutron star binaries by a factor of about 10, no Be + white dwarf system has ever been confirmed so far. This absence casts some doubts on our current understanding of massive X-ray binary evolution. The goal of the proposed observation is to characterize the X-ray spectral and temporal properties of these X-ray emitters and search for the signatures of an accreting white dwarf.

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