Physics
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1864p&link_type=abstract
IUE Proposal ID #CBGMP
Physics
Scientific paper
I propose to exploit the discovery of the circumstellar hot turbulent shell surrounding the gainers in some of the semidetached binaries of the Algol type (henceforth briefly the Algols.) This shell radiates in emission lines of fairly high ionization (ref. 1, 2, 3), but can also be observed in absorption when highdispersion IUE spectra are used (ref. 3; Peters and Polidan, preprint). The high temperature (60,000 - 120,000 K) and turbulent character of the shell suggest that it takes its energy from the accretion process. Its large extent and the P Cygni character of the emissions (seen in high-dispersion spectra) indicate mass outflow from the system. The shell is present in all W Serpentis stars (ref. 7) and has been detected in about six "classical" Algols. What is the importance of the shell? (1) It is an important part of the mass transfer/accretion/mass loss process. (2) From the relative line intensities, we can study the C/N abundance ratio and determine the extent to which the material was subject to CNO-processing in the core of the loser. I propose to observe selected Algol systems in primary eclipses in order to detect the shell and derive its physical properties and chemical abundances. An attempt will be made to find a correlation between the presence, extent, and characteristics of the shell and the system parameters. Low-dispersion SWP spectra of the selected systems in eclipses can be obtained in US2 shifts. An analysis of the profiles of the absorption lines formed in the shell is possible for a few of the selected systems if high-dispersion SWP spectra are obtained; these require one US1 shift.
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