Resolving the puzzling nature of the ultra-compact binary V407 Vul

Details Resolving the puzzling nature of the ultra-compact binary V407 Vul Resolving the puzzling nature of the ultra-compact binary V407 Vul

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008hst..prop11627n&link_type=abstract

HST Proposal ID #11627. Cycle 17

Computer Science

Scientific paper

Recently, three variable stars have been identified as likely accreting binary systems with ultra-short orbital periods of 10 minutes or less. This makes them the closest binaries known as well as strong sources of gravitational wave emission. These objects have thus been identified as crucial calibration sources for the LISA mission. V407 Vul diplays a 9.5 minute period at optical and X-ray wavelengths. Several different binary geometries have been proposed to explain this variable star with all but one scenario identifying the 9.5 minute period with the binary orbital period. Our time-resolved spectroscopy and photometry from the ground revealed that the optical light is dominated by a stationary G9 star which would be inconsistent with the mass donor star of a compact binary. We propose ACS/HRC imaging in order to confirm the tentative 0.03" mis-alignment we have picked up between this G9 star and the underlying variable. Confirmation of a spatial separation between the variable and this field star would conclusively rule out that the G star is part of a low-inclination binary and thus verify it as a LISA source. In addition, we propose UV imaging that will allow us to determine the NUV luminosity of the variable star and thereby reliably infer the distance and the nature {and thus the gravitational wave signal} of the ultra-compact binary, as either mass transfer or magnetic interaction powers the X-ray source. Only HST imaging can provide rigorous proof for an ultra-compact binary interpretation for V407 Vul and thus validate it as LISA verification source;

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