Gravitational Wave Heating of Stars and Accretion Disks
  We investigate the electromagnetic (EM) counterpart of gravitational waves
(GWs) emitted by a supermassive black hole binary (SMBHB) through the viscous
dissipation of the GW energy in an accretion disk and stars surrounding the
SMBHB. We account for the suppression of the heating rate if the forcing period
is shorter than the turnover time of the largest turbulent eddies. We find that
the viscous heating luminosity in 0.1 solar mass stars can be significantly
higher than their intrinsic luminosity, but still too low to be detected for
extragalactic sources. The relative brightening is small for accretion disks.
