Evolution of the Symbiotic Nova AG Pegasi

Details Evolution of the Symbiotic Nova AG Pegasi Evolution of the Symbiotic Nova AG Pegasi

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8369k&link_type=abstract

HST Proposal ID #8369

Computer Science

Hst Proposal Id #8369 Binary Stars

Scientific paper

We propose to study high signal-to-noise FOS and GHRS observations of the symbiotic nova AG Pegasi. We plan to analyze the ultraviolet spectra together with contemporaneous low resolution optical spectrophotometry of similarly high quality. These data will allow us to examine the line and continuum fluxes and radial velocities at several orbital phases for species with ionization potentials ranging from 10 eV up to 100 eV. We expect three main results from this program. {i} Orbital modulation of the emission line fluxes will yield a better understanding of the geometry of the ionized wind of the red giant primary star. This result will test our predictions that low ionization lines form near the red giant photosphere and that higher ionization species lie close to the accreting white dwarf companion. {ii} Emission line radial velocities will help to constrain the wind geometry and may place limits on the mass of the white dwarf. {iii} The continuum and emission line fluxes will test predictions of our non-LTE photoionization code. We have derived order-of-magnitude estimates for the mass loss rate in the red giant wind and placed some limits on the velocity law in this wind from archival IUE spectra. The HST data will yield better constraints on these wind parameters and begin to test hydrodynamical models for wind accretion in detached binaries.

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