  We numerically investigate the internal evolution of multiphase clouds, which
are at rest with respect to an ambient, highly ionized medium (HIM)
representing the hot component of the circumgalactic medium (CGM).
Time-dependent saturated thermal conduction and its implications like
condensation rates and mixing efficiency are assessed in multiphase clouds. Our
simulations are carried out by using the adaptive mesh refinement code Flash.
We perform a grid of models of which we present here those characteristic for
the presented study. The model clouds are initially in both hydrostatic and
thermal equilibrium and are in pressure balance with the HIM. Thus, they have
steep gradients in both temperature and density at the interface to HIM leading
to non-negligible thermal conduction. Several physical processes are considered
numerically or semi-analytically: thermal conduction, radiative cooling and
external heating of gas, self-gravity, mass diffusion, and dissociation of
molecules and ionization of atoms. It turns out that saturated thermal
conduction triggers a continuous condensation irrespective of cloud mass.
Dynamical interactions with ambient HIM all relate to the radial density
gradient in the clouds: (1) mass flux due to condensation is the higher the
more homogeneous the clouds are; (2) mixing of condensed gas with cloud gas is
easier in low-mass clouds, because of their shallower radial density gradient;
thus (3) accreted gas is distributed more efficiently. A distinct and
sub-structured transition zone forms at the interface between cloud and HIM,
which starts at smaller radii and is much narrower as deduced from analytical
theory.
