We examine how different viscosity prescriptions and magnitudes affect the
structure of the slim disk. Unlike the case with a standard disk, radiation
from the slim disk is influenced by the viscosity parameter, alpha, in suc
h a way that the estimated maximum effective temperature of the disk slight
ly increases as alpha increases. This is because the larger is alpha, the l
arger does the accretion velocity become and, hence, the more enhanced does
the advective energy transport become, which means less efficient radiativ
e cooling and thus higher temperatures. Furthermore, we checked different v
iscosity prescriptions with the form of the viscous stress tensor of t(r ph
i) = -alpha beta (mu)p(total), where beta is the ratio of the gas pressure
to the total pressure, and mu is a parameter (0 less than or equal to mu le
ss than or equal to 1). In contrast with the case with It = 0, which shows
significant decrease in the inner-edge radius and the flattering of the eff
ective temperature profile at high luminosities, for large mu, say mu simil
ar to 0.5, neither of the inner-edge of the disk nor temperature profiles d
oes not appreciably change even at the Eddington luminosity. We can rule ou
t a case with large mu (similar to 0.5), since it would not be able to prod
uce a drop in the inner-edge radius of an increase in the luminosity, as wa
s observed in an ultraluminous X-ray source, IC 342, source 1.