The stellar wind of hot subdwarf stars

Details The stellar wind of hot subdwarf stars The stellar wind of hot subdwarf stars

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010xmm..prop...57l&link_type=abstract

XMM-Newton Proposal ID #06713901

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Stars, White Dwarfs, Solar System, Bd+37 442

Scientific paper

All we know about hot subdwarf (sd) stars is based on studies in the optical and UV domain, while none of them has been detected at X-rays. The only exception is the sdO binary HD49798, in which the WD companion shows a significant X-ray emission, due to the matter accreted from the sd primary. A recent XMM observation of this source has revealed a significant X-ray emission also during the eclipse phase, when the WD is obscured by the primary subdwarf, thus suggesting that the observed X-ray flux is due to the subdwarf itself. In order to investigate if also other sdO stars are characterized by an intrinsic X-ray emission, we propose to observe BD+37 442: it is a nearby and bright sdO star with a strong stellar wind, therefore it is the best candidate to perform this type of search.

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