The close-in extrasolar giant planets [CEGPs], \ltorder 0.05 AU from their
parent stars, may have a large component of optically reflected light. We
present theoretical optical photometric light curves and polarization curves
for the CEGP systems, from reflected planetary light. Different particle sizes
of three condensates are considered. In the most reflective case, the
variability is ≈100 micromagnitudes, which will be easily detectable
by the upcoming satellite missions MOST, COROT, and MONS, and possibly from the
ground in the near future. The least reflective case is caused by small, highly
absorbing grains such as solid Fe, with variation of much less than one
micromagnitude. Polarization for all cases is lower than current detectability
limits. We also discuss the temperature-pressure profiles and resulting
emergent spectra of the CEGP atmospheres. We discuss the observational results
of Tau Boo b by Cameron et al. (1999) and Charbonneau et al. (1999) in context
of our model results. The predictions - the shape and magnitude of the light
curves and polarization curves - are highly dependent on the size and type of
condensates present in the planetary atmosphere.Comment: 33 pages, accepted by Ap