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We report optical photometric observations of four superoutbursts of theshort-period dwarf nova TV Crv. This object experiences two types ofsuperoutbursts; one with a precursor and the other without. The superhumpperiod and period excess of TV Crv are accurately determined to be 0.065028 +/-0.8 d and 0.0342 +/- 0.0021, respectively. This large excess implies arelatively large mass ratio of the binary components (M_2/M_1), though it has ashort orbital period. The two types of superoutbursts can be explained by thethermal-tidal instability model for systems having large mass ratios. Ourobservations reveal that superhump period derivatives are variable in distinctsuperoutbursts. The variation is apparently related to the presence or absenceof a precursor. We propose that the superhump period derivative depends on themaximum disk radius during outbursts. We investigate the relationship of thetype of superoutbursts and the superhump period derivative for known sources.In the case of superoutbursts without a precursor, superhump period derivativestend to be larger than those in precursor-main type superoutbursts, which isconsistent with our scenario.Comment: 13 pages, 11 figures, accepted for publication in A&

TV Corvi revisited: Precursor and superhump period derivative linked to the disk instability model