  We studied global nonaxisymmetric hydrodynamic instabilities in an extensive
collection of hot, self-gravitating polytropic disk systems, systems that
covered a wide expanse of the parameter space relevant to protostellar and
protoplanetary systems. We examined equilibrium disk models varying three
parameters: the ratio of the inner to outer equatorial radii, the ratio of star
mass to disk mass, and the rotation law exponent $q$. We took the polytropic
index $n$ = 1.5 and examined the exponents $q =$ 1.5 and 2, and the
transitional one $q$ = 1.75. For each of these sets of parameters, we examined
models with inner to outer radius ratios from 0.1 to 0.75, and star mass to
disk mass ratios from 0 to 10$^3$. We numerically calculated the growth rates
and oscillation frequencies of low-order nonaxisymmetric disk modes, modes with
azimuthal dependence $\propto$ e$^{im\phi}$. Low-$m$ modes are found to
dominate with the character and strength of instability strongly dependent on
disk self-gravity. Representatives of each mode type are examined in detail,
and torques and mass transport rates are calculated.
