  We present calculations for the evolution and surviving mass of
highly-irradiated extrasolar giant planets (EGPs) at orbital semimajor axes
ranging from 0.023 to 0.057 AU using a generalized scaled theory for mass loss,
together with new surface-condition grids for hot EGPs and a consistent
treatment of tidal truncation. Theoretical estimates for the rate of
energy-limited hydrogen escape from giant-planet atmospheres differ by two
orders of magnitude, when one holds planetary mass, composition, and
irradiation constant. Baraffe et al. (2004, A&A 419, L13-L16) predict the
highest rate, based on the theory of Lammer et al. (2003, Astrophys. J. 598,
L121-L124). Scaling the theory of Watson et al. (1981, Icarus 48, 150-166) to
parameters for a highly-irradiated exoplanet, we find an escape rate ~102 lower
than Baraffe's. With the scaled Watson theory we find modest mass loss,
occurring early in the history of a hot EGP. In this theory, mass loss
including the effect of Roche-lobe overflow becomes significant primarily for
masses below a Saturn mass, for semimajor axes = 0.023 AU. This contrasts with
the Baraffe model, where hot EGPs are claimed to be remnants of much more
massive bodies, originally several times Jupiter and still losing substantial
mass fractions at present.
