Dissecting the Wind and Disk of the Nova-like Variable V347 Puppis

Details Dissecting the Wind and Disk of the Nova-like Variable V347 Puppis Dissecting the Wind and Disk of the Nova-like Variable V347 Puppis

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6546m&link_type=abstract

HST Proposal ID #6546

Physics

Hst Proposal Id #6546 Binaries And Star Formation

Scientific paper

As evidenced by the P Cygni profiles of their ultraviolet resonance lines, high mass accretion rate CVs suffer mass loss in the form of high-velocity winds. Models of these line profiles are consistent with a disk origin of these winds, and hence demonstrate a close link between mass accretion and mass loss in CVs, just as applies in AGN and protostars. Our understanding of CVs has been advanced in unique and important ways by observations of systems in which the secondary eclipses the disk and wind. Such observations constraint the geometry and kinematics of the wind, provide the full spectral energy distribution across the face of the disk, allow an assessment of the contributions to the observed line profiles and continuum by the disk, the hot spot, and the heated face of the secondary. With its long period, high inclination, strong UV emission lines, and weak UV continuum, the bright nova-like variable V347 Pup is an ideal system in which to perform these studies. Recent optical and IUE observations reveal variations in the lines and continuum at all orbital phases including eclipse. Recent theoretical studies of the wind make a number of predictions which can be tested only with the large collecting area and high spectral and temporal resolution of HST. We propose to test these predictions and to perform the above disk and wind studies via simultaneous phase-resolved measurements with the FOS/BL G130H grating of the N V, Si IV, and C IV emission lines and 1140-1606 Angstrom continuum of V347 Pup.

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