Time-resolved ultraviolet spectroscopy of the compact interacting binary QU Car

We present HST/STIS (1160--1700A) echelle spectra of the cataclysmic variable (CV) star, QU Car, observed in time-tag mode at three epochs. In catalogues this binary is classified as a nova-like variable. We find evidence of a high-state non-magnetic CV at low inclination, with unusually high ionisation. We observed narrow absorption lines (few hundred km/s wide) in N V1240, O V1371 and Si IV1398, as well as broader (HWZI ~1000km/s) emission in C III1176, C IV1549 and He II1640, all with a superposed absorption component. High ionisation is indicated by the unusually string He II emission and the relative strength of the O V absorption line. The dereddened UV SED of, on average, -2.3 suggests that disc accretion dominates the spectral energy distribution. In two observations velocity shifting is noted in the absorption lines on a timescale long enough not to repeat within the ~2600-sec exposures. The absorption superposed on the C IV emission line moves coherently with the N V and Si IV absorption, suggesting the same origin for all absorption lines -- most likely to be in the accretion disc atmosphere. Weak blueshifted absorption in NV and C\IV provides evidence of an outflow component and we estimate a maximum outflow velocity of ~2000km/s. This may be linked to a wind launched from further out in the disc than is typically seen in those high-state non-magnetic CV whose wind speeds are observed to reach to >4000km/s. Unusually, three ionisation stages of carbon -- C II, C III and C IV -- are present in emission, with line width increasing with higher ionisation. The presence of C II in emission and the positive line-width/ionisation correlation is most easily reconciled with an origin in a disc chromosphere, beyond the influence of the EUV-emitting inner disc.