Abstract
The long-term, time-resolved CCD photometry of a dwarf nova, DI UMa, has revealed this object to be a peculiar SU UMa-type dwarf nova having both the shortest ever observed superhump period (0.0555 d) and a very short (25 d) supercycle length. These features make DI UMa the fourth established member of a recently discovered small group of dwarf novae, called ER UMa stars or RZ LMi stars, which are now believed to be SU UMa-type dwarf novae with exceptionally high mass-transfer rates. DI UMa in all respects resembles a peculiar dwarf nova RZ LMi, but is more extreme in its short superhump period. The high-incident discovery of objects with such an extreme combination of parameters, which can not be expected from the standard evolution of cataclysmic variables (CVs), should provide a unique tool in probing the long-debated problem concerning the origin of mass-transfer in CVs and a secular alteration between CV subclasses.
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