  Superoutbursts in WZ Sge-type dwarf novae (DNe) are characterized by both
early superhumps and ordinary superhumps originating from the 2:1 and 3:1
resonances, respectively. However, some WZ Sge-type DNe show a superoutburst
lacking early superhumps; it is not well established how these differ from
superoutbursts with an early superhump phase. We report time-resolved
photometric observations of the WZ Sge-type DN V627 Peg during its 2021
superoutburst. The detection of ordinary superhumps before the superoutburst
peak highlights that this 2021 superoutburst of V627 Peg, like that {in} 2014,
did not feature an early superhump phase. The duration of stage B superhumps
was slightly longer in the 2010 superoutburst accompanying early superhumps
than that in the 2014 and 2021 superoutbursts which lacked early superhumps.
This result suggests that an accretion disk experiencing the 2:1 resonance may
have a larger mass at the inner part of the disk and hence take more time for
the inner disk to become eccentric. The presence of a precursor outburst in the
2021 superoutburst suggests that the maximum disk radius should be smaller than
that of the 2014 superoutburst, even though the duration of quiescence was
longer than that before the 2021 superoutburst. This could be accomplished if
the 2021 superoutburst was triggered as an inside-out outburst or if the mass
transfer rate in quiescence changes by a factor of two, suggesting that the
outburst mechanism and quiescence state of WZ Sge-type DNe may have more
variety than ever thought.
