FUV Emission Line Profiles of W Serpentis Binaries: Cycle 1 Observations

Details FUV Emission Line Profiles of W Serpentis Binaries: Cycle 1 Observations FUV Emission Line Profiles of W Serpentis Binaries: Cycle 1 Observations

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991hst..prop.1190b&link_type=abstract

HST Proposal ID #1190

Physics

Hst Proposal Id #1190

Scientific paper

We propose to use the HRS at intermediate resolution for the study of FUV emission line profiles in W Serpentis (which is the prototype of the 'W Serpentis' class of interacting binaries). The FUV spectrum of the W Ser systems is characterized by strong emissions at N V 1240, CII 1335, Si IV 1400, Si II 1533, C IV 1550 and Al II 1670. In cycle 1, we will concentrate on observations of the Si IV 1400 doublet in W Ser. Although these lines may be observed with IUE at low dispersion, all profile information is lost at this resolution, and the W Ser systems in general are too faint to be observed at IUE high dispersion. The emission lines are believed to arise from a high excitation wind powered by the accretion process. Modelling of observed line profiles will yield information about the physical properties of the mass outflow in these systems, as well as providing insight into a stage of evolution which many close binaries appear to undergo.

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