Analysis of the Si IV ultraviolet spectra of U Sagittae

Archival IUE spectra of U Sge have been used to study hot (similar to 10(5) K) circumstellar gas in this system. The observed spectra contain several UV resonance lines, of which the Si Iv lines (lambda lambda 1394 and 1405) are the strongest. These lines are observed in absorption, so we must remov e the photospheric absorption line contribution to the spectra in order to see the emission produced by the circumstellar gas. We have developed a rob ust method for creating such difference spectra from IUE data. In the obser ved spectra we see a variation in the line profiles and line centers with a n orbital phase suggesting the presence of circumstellar gas. The residual emission seen in the difference spectra is strongest between phases phi = 0 .3 and phi = 0.7, with a strength of up to 0.2 of the continuum flux. This is confirmed by the presence of an emission region visible in the Doppler t omogram of the lambda 1394 line. This is consistent with the location of an H alpha "absorption zone" seen in tomograms of U Sge and U CrB, and with t heoretical predictions of a high temperature accretion region.