  We observed the 1998 November superoutburst of WX Cet, a dwarf nova
originally proposed as a WZ Sge-like system. The observation established that
WX Cet is an SU UMa-type dwarf nova with a mean superhump period of 0.05949(1)
d, which is 2.1% longer than the reported orbital period. The lack of early
superhumps at the earliest stage of the superoutburst, the rapid development of
usual superhumps, and the possible rapid decay of late superhumps seem to
support that WX Cet is a fairly normal large-amplitude SU UMa-type dwarf nova,
rather than a WZ Sge-type dwarf nova with a number of peculiarities. However, a
period increase of superhumps at a rate dot(P)/P = (+8.5+/-1.0) x 10^-5 was
observed, which is one of the largest dot(P)/P ever observed in SU UMa-type
dwarf novae. A linear decline of light, with a rate of 0.10 mag/d, was observed
in the post-superoutburst stage. This may be an exemplification of the decay of
the viscosity in the accretion disk after the termination of a superoutburst,
mechanism of which is proposed to explain a variety of post-superoutburst
phenomena in some SU UMa-type dwarf novae.
