We report 1992-1999 photometry of the helium-rich cataclysmic variable V803
Centauri. In its high brightness state at V = 13, the star shows a strong
periodic signal with P = 1618 s; this resembles the superhumps associated w
ith many dwarf novae. However, it is unusual because the superhump appears
to endure through all brightness states, including the very faint state at
V = 17. The star also becomes occasionally stuck in a "cyclingstate," in wh
ich the brightness varies in the range 13.4-14.5, with a period of 22 +/- 1
hr. This appears to be the recurrence pattern of " normal " dwarf nova out
bursts. Thus the underlying physics is probably that of a dwarf nova, but w
ith an accretion disk dominated by helium. Reckoned as a dwarf nova, V803 C
en presents an interesting test for accretion disk, theory, because it appe
ars to display two timescales for eruption recurrence: 0.94 day at V = 14.5
and similar to 5 days at V = 17.2. This is roughly consistent with the gen
eral idea that recurrence time scales inversely with accretion rate.