  We present the results of a long ROSAT HRI observation of the candidate
intermediate polar TW Pic. The power spectrum shows no sign of either the
previously proposed white dwarf spin period or the proposed binary orbital
period (1.996 hr and 6.06 hr respectively). The limits to the X-ray modulation
are less than 0.3% in each case. In the absence of a coherent X-ray pulsation,
the credentials of TW Pic for membership of the intermediate polar subclass
must be suspect. We further suggest that the true orbital period of the binary
may be the shorter of the two previously suggested, and that the longer period
may represent a quasi-periodic phenomenon associated with the accretion disc.
