  According to a generalization of black hole thermodynamics to a cosmological
framework, it is possible to define a temperature for the cosmological horizon.
The hypothesis of thermal equilibrium between the dark energy and the horizon
has been considered by many authors. We find the restrictions imposed by this
hypothesis on the energy transfer rate ($Q_i$) between the cosmological fluids,
assuming that the temperature of the horizon have the form $T=b/2\pi R$, where
$R$ is the radius of the horizon. We more specifically consider two types of
dark energy: holographic dark energy (HDE) and dark energy with a constant EoS
parameter ($w$DE). In each case, we show that for a given radius $R$, there is
an unique term $Q_{de}$ that is consistent with thermal equilibrium. We also
consider the situation where, in addition to dark energy, other fluids (cold
matter, radiation) are in thermal equilibrium with the horizon. We find that
the interaction terms required for this will generally violate energy
conservation ($\sum_i Q_i=0$).
