Mass flow in the interacting binary TX Ursae Majoris

Details Mass flow in the interacting binary TX Ursae Majoris Mass flow in the interacting binary TX Ursae Majoris

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281a.201m&link_type=abstract

In ESA, A Decade of UV Astronomy with the IUE Satellite, Volume 1 p 201-203 (SEE N89-10682 01-89)

Astronomy and Astrophysics

Astronomy

3

Eclipsing Binary Stars, Iue, Mass Flow, Spaceborne Astronomy, Stellar Mass, Ultraviolet Astronomy, Ultraviolet Spectra, Gas Flow, Radial Velocity, Stellar Envelopes

Scientific paper

Twenty-two far-ultraviolet and 23 near-ultraviolet high resolution IUE spectra of the interactive Algol-type binary TX Ursae Majoris (B8 V + F-K III-IV) were analyzed in order to determine the nature of the mass flow occurring in this system. Absorption features due to high-temperature ions of Si IV, C IV, and N V are always present. The resonance lines of Al III, Fe II, Mg II and Si IV show strong phase and secular variations indicative of gas streaming and circumstellar/circumbinary material. Radial velocities as high as 500 to 600 km/sec are present. The gas flow is particularly prominent in 1985 between phases 0.7 and 0.0. The system is more active than U Sagittae and as active as U Cephei.

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