We present high resolution Hubble Space Telescope ultraviolet spectroscopy of the dwarf nova EK TrA obtained in deep quiescence .
The Space Telescope Imaging Spectrograph data reveal the broad { Ly \alpha } absorption profile typical of a moderately cool white dwarf , overlayed by numerous broad emission lines of He , C , N , and Si and by a number of narrow absorption lines , mainly of C I and Si II .
Assuming a white dwarf mass in the range 0.3 - 1.4 M _ { \odot } we derive \mbox { $T _ { eff } $ } = 17 500 - 23 400 K for the primary in EK TrA ; \mbox { $T _ { eff } $ } = 18 800 K for a canonical mass of 0.6 M _ { \odot } .
From the narrow photospheric absorption lines , we measure the white dwarf rotational velocity , v \sin i = 200 \pm 100 km s ^ { -1 } .
Even though the strong contamination of the photospheric white dwarf absorption spectrum by the emission lines prevents a detailed quantitative analysis of the chemical abundances of the atmosphere , the available data suggest slightly sub-solar abundances .
The high time resolution of the STIS data allows us to associate the observed ultraviolet flickering with the emission lines , possibly originating in a hot optically thin corona above the cold accretion disk .