  RZ Psc is a young Sun-like star, long associated with the UXor class of
variable stars, which is partially or wholly dimmed by dust clumps several
times each year. The system has a bright and variable infrared excess, which
has been interpreted as evidence that the dimming events are the passage of
asteroidal fragments in front of the host star. Here, we present a decade of
optical photometry of RZ Psc and take a critical look at the asteroid belt
interpretation. We show that the distribution of light curve gradients is
non-uniform for deep events, which we interpret as possible evidence for an
asteroidal fragment-like clump structure. However, the clumps are very likely
seen above a high optical depth mid-plane, so the disk's bulk clumpiness is not
revealed. While circumstantial evidence suggests an asteroid belt is more
plausible than a gas-rich transition disk, the evolutionary status remains
uncertain. We suggest that the rarity of Sun-like stars showing disk-related
variability may arise because i) any accretion streams are transparent, and/or
ii) turbulence above the inner rim is normally shadowed by a flared outer disk.
