Unveiling the nature of the 321s orbital period binary RXJ0806.3+1527

Details Unveiling the nature of the 321s orbital period binary RXJ0806.3+1527 Unveiling the nature of the 321s orbital period binary RXJ0806.3+1527

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004hst..prop10218i&link_type=abstract

HST Proposal ID #10218

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Hst Proposal Id #10218 Hot Stars

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This porposal is aimed at studying one of the potentially most important binary system in our Galaxy, namely RXJ0806.3+1527. Our group discovered a 321s periodic modulation in its optical and X-ray flux and we poposed that it originates form the orbital motion {the shortest known} of a white dwarf around another lighter white dwarf. VLT optical spectra showed faint and broad {1500km/s FWHM} HeII {mainly} emission lines, even though the presence of H can not be completely ruled out due to spectral resolution. Moreover, recent XMM observations with the OM confirmed that the broad band energy spectrum of this source peaks in the UV band, making it one of the best target for HST studies. Here we propose to use the STIS spectroscopic capability of HST in the TIME-TAG mode. The latter mode is extremely well suited for our purposes, since will allow us, among other things, to perform, for the first time, an Orbital Phase Spectroscopy of the expected He lines {also those of C, N and O are expected} in the STIS spectra. We expect to finally probe the nature of the source by following the emission line centroid shift as a function of the orbital phase, making RXJ0806.3+1527 a single-component spectroscopic binary and opening a new perspective in the field of double degenerate systems {the emission lines of the greatest part of which are dominated by the effect of the disk rotation}.

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