  Interacting binaries in which a white dwarf accretes material from a
companion --- cataclysmic variables (CVs) in which the mass loss is via
Roche-lobe overflow, and symbiotic stars in which the white dwarf captures the
wind of a late type giant --- are relatively commonplace. They display a wide
range of behaviors in the optical, X-rays, and other wavelengths, which still
often baffles observers and theorists alike. They are likely to be a
significant contributor to the Galactic ridge X-ray emission, and the
possibility that some CVs or symbiotic stars may be the progenitors of some of
the Type Ia supernovae deserves serious consideration. Furthermore, these
binaries serve as excellent laboratories in which to study physics of X-ray
emission from high density plasma, accretion physics, reflection, and particle
acceleration. ASTRO-H is well-matched to the study of X-ray emission from many
of these objects. In particular, the excellent spectral resolution of the SXS
will enable dynamical studies of the X-ray emitting plasma. We also discuss the
possibility of identifying an accreting, near-Chandrasekhar-mass white dwarf by
measuring the gravitational redshift of the 6.4 keV line.
