  We report on time-resolved photometric observations of the WZ Sge-type dwarf
nova, EG Cnc (Huruhata's variable, see also
http://www.kusastro.kyoto-u.ac.jp/vsnet/DNe/egcnc.html), during its
superoutburst in 1996-1997. EG Cnc, after the main superoutburst accompanied
with development of superhumps typical of a WZ Sge-type dwarf nova, exhibited a
series of six major rebrightenings. During these rebrightenings and the
following long fading tail, EG Cnc persistently showed superhumps having a
period equal to the superhump period observed during the main superoutburst.
The persistent superhumps had a constant superhump flux with respect to the
rebrightening phase. These findings suggest the superhumps observed during the
rebrightening stage and the fading tail are a "remnant" of usual superhumps,
and are not newly triggered by rebrightenings. By comparison with the 1977
outburst of this object and outbursts of other WZ Sge-type dwarf novae, we
propose an activity sequence of WZ Sge-type superoutbursts, in which the
current outburst of EG Cnc is placed between a single-rebrightening event and
distinct outbursts separated by a dip. The post-superoutburst behavior of WZ
Sge-type dwarf novae can be understood in the presence of considerable amount
of remnant matter behind the cooling front in the outer accretion disk, even
after the main superoutburst. We consider the premature quenching of the hot
state due to the weak tidal effect under the extreme mass ratio of the WZ
Sge-type binary is responsible for the origin of the remnant mass.
