SIMBAD references

The IUE archive contains numerous low resolution spectra of dwarf novae in outburst but relatively little synthetic spectral analyses of them using realistic accretion disk models with spectral lines. We have examined a series of previously unstudied archival IUE low resolution SWP spectra of the SU UMa-type ultra-short period dwarf nova T Leonis, obtained continously through a single dwarf nova outburst. We describe its outburst spectra, characterizing its metallic absorption line spectrum, and the shape of its energy distribution. We estimate a terminal wind velocity of 2500 km/s, and report posible evidence of wind variability on timescales of roughly 2 hours, although orbital pahse variations cannot be ruled out. We have constructed a grid of optically thick accretion disk models for white dwarf masses 0.6 and 1.0 M_☉ , accretion rates 10^{-11} to 10^{-7} M_☉/year, and for disk inclination angles of 40^ø and 80^ø. We carry out preliminary synthetic accretion disk spectral fitting of T Leonis and present the results. Our best-fitting model to a coaddition of three spectra with similar S/N yields M_{wd} = 0.6 M_☉, i ≃40^ø, {dot}M ≃10^{-9}M_☉/yr with an inner disk temperature of 30,000 K and an outer disk temperature of 14,000 K. These results compare favorably with analyses of optical spectra of T Leonis in outburst, suggesting that a similar application to other far UV spectra of dwarf novae in outburst, with a finer grid of disk models, should prove profitable.(c) Astronomical Society of the Pacific