Accretion disks are ubiquitous in our universe, and produce intense
brightening. How does the gas in the disk lose its angular momentum
to release massive amounts of gravitational energy? This is one of
the biggest open questions in astronomy. This book studies four
types of newly detected outbursts in dwarf novae through optical
observations and/or numerical simulations and puts forward physical
interpretations of these outbursts on the basis of the disk
instability model, the most plausible model for dwarf-nova
outbursts. It demonstrates that the disk-instability model can
explain rich variety in dwarf-nova outbursts if some new aspects
are taken into account (e.g. the extremely slow growth of tidal
instability and thermal instability in the disk misaligned against
the binary orbital plane). Moreover, it shares valuable insights on
the evolution of binary systems by finding period bouncers and
dwarf novae with F-type companion stars, which are rare objects.
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