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- W2142428079 abstract "Archival IUE spectra of U Sge have been used to study hot (D105 K) circumstellar gas in this system. The observed spectra contain several UV resonance lines, of which the Si IV lines (jj1394 and 1405) are the strongest. These lines are observed in absorption, so we must remove the photospheric absorption line contribution to the spectra in order to see the emission produced by the circumstellar gas. We have developed a robust method for creating such diUerence spectra from IUE data. In the observed spectra we see a variation in the line pro—les and line centers with an orbital phase suggesting the presence of circumstellar gas. The residual emission seen in the diUerence spectra is strongest between phases / 0.3 and / 0.7, with a strength of up to 0.2 of the continuum —ux. This is con—rmed by the presence of an emission region visible in the Doppler tomogram of the j1394 line. This is consistent with the location of an Ha ii absorption zone ˇˇ seen in tomograms of U Sge and U CrB, and with theoretical predictions of a high temperature accretion region. Subject headings : accretion, accretion disksbinaries : eclipsingcircumstellar matter ¨ stars : individual (U Sagittae) ¨ ultraviolet : stars" @default.
- W2142428079 created "2016-06-24" @default.
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- W2142428079 date "1999-02-10" @default.
- W2142428079 modified "2023-09-27" @default.
- W2142428079 title "Analysis of the SiivUltraviolet Spectra of U Sagittae" @default.
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- W2142428079 doi "https://doi.org/10.1086/306774" @default.
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