  Motivated by observations of multiphase galaxy outflows, we explore the
impact of isotropic and anisotropic electron thermal conduction on the
evolution of radiatively-cooled, cold clouds embedded in hot, magnetized winds.
Using the adaptive mesh refinement code AthenaPK, we conduct simulations of
clouds impacted by supersonic and transonic flows with magnetic fields
initially aligned parallel and perpendicular to the flow direction. In cases
with isotropic thermal conduction, an evaporative wind forms, stabilizing
against instabilities and leading to a mass loss rate that matches the
hydrodynamic case. In anisotropic cases, the impact of conduction is more
limited and strongly dependent on the field orientation. In runs with initially
perpendicular fields, the field lines are folded back into the tail, strongly
limiting conduction, but magnetic fields act to dampen instabilities and slow
the stretching of the cloud in the flow direction. In the parallel case,
anisotropic conduction aids cloud survival by forming a radiative wind near the
front of the cloud, which suppresses instabilities and reduces mass loss. In
all cases, anisotropic conduction has a minimal impact on the acceleration of
the cloud.
