Several models are calculated in order to assess the effects of differ
ent physical parameters on the thermal evolution of Venus. The models
are based on three-dimensional thermal convection calculations in an i
ncompressible mantle of infinite Prandtl number using a modified Bouss
inesq approximation. The mantle is assumed to have a temperature- and
pressure-dependent viscosity, temperature-dependent thermal conductivi
ty, depth-dependent thermal expansion coefficient, and time-dependent
internal heat generation rate. The physical parameters considered are
the initial temperature distribution, a possible D''-like layer at the
base of the mantle, the temperature at the core/mantle boundary, the
core solidification, the decrease of thermal expansion coefficient wit
h depth, the rate of internal heat generation, the radially dependent
viscosity, and the velocity boundary condition at the surface. A const
ant temperature at the core/mantle boundary develops a strong thermal
boundary layer at the base of the mantle, resulting in highly oscillat
ory mantle convection. Allowing the core to cool suppresses the bounda
ry layer and reduces the amplitude of the oscillations substantially.
The initial temperature distribution, the core solidification, and a D
''-like layer have minor effects on the overall cooling of the mantle,
although the enhanced heat of fusion of the core hampers the cooling
of the core. The decrease of the thermal expansion coefficient with de
pth lowers the slope of the adiabatic temperature gradient in the mant
le and reduces the temperature in the lower part of the mantle and the
core appreciably. The heat generation rate has a significant effect o
n the present thermal state of the mantle; a higher rate of heat gener
ation enhances the mantle temperature. Similarly, a higher mantle visc
osity decreases the convection velocities and hampers the heat loss fr
om the mantle. However, the most important parameter that controls the
thermal evolution of the planet is the velocity boundary condition at
the surface. A stress-free (we examined semifree) surface allows mant
le material to approach the surface and coal efficiently, whereas a ri
gid (we examine semirigid) surface hampers heat loss from the planet,
resulting in a hot planet even when the internal heat sources are redu
ced by about an order of magnitude.