Determining the physical parameters of AM CVn binaries

Details Determining the physical parameters of AM CVn binaries Determining the physical parameters of AM CVn binaries

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006xmm..prop...87r&link_type=abstract

XMM-Newton Proposal ID #05023503

Computer Science

Stars, White Dwarfs, Solar System, V803 Cen, Sdss J1411+48, Xmm-Newton Proposal 05023503

Scientific paper

AM CVn binaries are a group of stars in which a white dwarf accretes from a hydrogen deficient companion in a very short period binary (P_orb=5-65 mins). We can study accretion flows of almost pure helium. They are predicted to be strongest known sources for the gravitational wave observatory LISA. We aim to extend our survey of these objects using XMM which has shown that a large fraction of their accretion luminosity is emitted in the UV and X-ray bands. In particular, we will determine the mass transfer rate, the element abundance from their X-ray spectra and characterise the X-ray and UV variability for 4 systems. Together with our existing dataset of these systems it will give us important clues for our understanding of their evolutionary history and their energy balance.

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