Mass loss in the interacting semi-detached binary delta librae

Details Mass loss in the interacting semi-detached binary delta librae Mass loss in the interacting semi-detached binary delta librae

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995lehi.reptq....m&link_type=abstract

Final Report Lehigh Univ., Bethlehem, PA. Dept. of Mathematics.

Mathematics

Eclipsing Binary Stars, Mass Flow, Stellar Spectra, Ultraviolet Spectroscopy, High Resolution, Iue, Line Spectra, Photosphere, Radial Velocity, Spectrum Analysis, Stellar Envelopes

Scientific paper

The interacting Algol-type binary Delta Librae (AOV + G: V) has been observed with the International Ultraviolet Explorer (IUE) satellite. More than fifty high resolution spectra in the far-ultraviolet and mid-ultraviolet spectrum have been analyzed in order to model the mass flow in the Delta Librae system. The resonance lines of Si IV and C IV are present in absorption and vary in strength both secularly and with phase. The radial velocities of the Si IV and C IV absorption lines generally follow the orbital motion of the primary star but deviate by typically a few tens of kilometers per second in the direction of the observer. The presence of Si IV and C IV features indicates the existence of a region considerably hotter than the normal AOV photosphere and, since these lines are present at all phases, this region must be fairly extensive. These results are interpreted in terms of a 'pseudo-photosphere' around the equatorial region of the AOV star, created by matter being accreted from the G-type companion. The widths of the Si IV and C IV absorption features imply that some of the matter lost by the G-star leaves the system entirely.

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