The Onset of Wolf-Rayet-Like Wind Outflow from the Hot Component in the Symbiotic Nova PU VUL

Details The Onset of Wolf-Rayet-Like Wind Outflow from the Hot Component in the Symbiotic Nova PU VUL The Onset of Wolf-Rayet-Like Wind Outflow from the Hot Component in the Symbiotic Nova PU VUL

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...18110213s&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #102.13; Bulletin of the American Astronomical Society, Vol. 24, p.1286

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We have analyzed temporal variations in the far ultraviolet He II (1640), Si IV (1393, 1402), and C IV (1548, 1550) line profiles in eight high dispersion IUE\ SWP spectra of the symbiotic nova PU Vul by comparatively examining these profiles on a common velocity scale. We see clear evidence of the onset of a Wolf-Rayet-like wind outflow from the bloated, contracting white dwarf hot component with terminal velocity of -550 to -600 km/s. The profile interpretations are complicated by the presence of superposed discrete absorption components due to partial obscuration of the outflow by lowly ionized Fe-peak absorbers in the foreground slow, cool, wind of the red giant component (Shore 1992). High resolution IUE\ spectra taken in 1990 and 1991, compared in velocity space to spectra obtained 1987-1990, reveal dramatic changes in the profiles with the development of a clear P Cygni structure, identical in velocity space for both components of Si IV (1393, 1402) as well as a large increase in the intensity of the broad He II emission (FWZI = ~ 900 km/s) wind profile. For a column density of material (10(22) /cm(2) ) obscuring the hot component we obtain a lower limit\ net He II emission line equivalent width of 1 Angstroms. As a preliminary attempt to constrain the mass loss rate, we compare the morphological structure of the He II (1640) wind profile with the theoretical He II (1640) Wolf-Rayet profiles of Hamann and Schutz (1987). Comparisons with hot component outflows in other symbiotic systems are discussed. This work is supported by NASA grants NAG5-343 and NAG5-1284 to Villanova University.

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