  The ROSAT WFC survey has provided us with evidence for the existence of a
previously unidentified sample of hot white dwarfs (WD) in non-interacting
binary systems, through the detection of EUV and soft X-ray emission. These
stars are hidden at optical wavelengths due to their close proximity to much
more luminous main sequence (MS) companions (spectral type K or earlier).
However, for companions of spectral type A5 or later the white dwarfs are
easily visible at far-UV wavelengths, and can be identified in spectra taken by
IUE. Eleven white dwarf binary systems have previously been found in this way
from ROSAT, EUVE and IUE observations (e.g. Barstow et al. 1994). In this paper
we report the discovery of three more such systems through our programmes in
recent episodes of IUE. The new binaries are HD2133, RE J0357+283 (whose
existence was predicted by Jeffries, Burleigh and Robb 1996), and BD+27 1888.
In addition, we have independently identified a fourth new WD+MS binary, RE
J1027+322, which has also been reported in the literature by Genova et al.
(1995), bringing the total number of such systems discovered as a result of the
EUV surveys to fifteen. We also discuss here six stars which were observed as
part of the programme, but where no white dwarf companion was found. Four of
these are coronally active. Finally, we present an analysis of the WD+K0IV
binary HD18131 (Vennes et al. 1995), which includes the ROSAT PSPC X-ray data.
