X-ray emission from hot subdwarfs with compact companions
1 INAF – IASF Milano, via Bassini 15, 20133 Milano, Italy
2 IUSS, piazza della Vittoria 15, 27100 Pavia, Italy
a e-mail: firstname.lastname@example.org
We review the X-ray observations of hot subdwarf stars. While no X-ray emission has been detected yet from binaries containing B-type subdwarfs, interesting results have been obtained in the case of the two luminous O-type subdwarfs HD 49798 and BD + 37° 442. Both of them are members of binary systems in which the X-ray luminosity is powered by accretion onto a compact object: a rapidly spinning (13.2 s) and massive (1.28 M⊙) white dwarf in the case of HD 49798 and most likely a neutron star, spinning at 19.2 s, in the case of BD + 37° 442. Their study can shed light on the poorly known processes taking place during common envelope evolutionary phases and on the properties of wind mass loss from hot subdwarfs.
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