New holographic dark energy and the modified Bekenstein-Hawking entropy
  We show that in the standard derivation of the holographic dark energy some
conceptual issues are present. In particular, the formula used in the
literature to avoid black holes is not suitable in expanding universes. A more
suitable expression for a holographic motivated dark energy must contain the
energy density of the remaining matter content of the universe. However, we
show that under some reasonable hypothesis, we can obtain a new physically
motivated expression for the holographic dark energy. By considering an
appropriate time-dependence of the saturation-level parameter, a de Sitter
phase arises. Moreover, by adopting an argument similar to the original
Bekenstein one, our approach justifies a correction of the Bekenstein-Hawking
entropy for non-static isotropic expanding universes. Finally, we write down
the equation of state of a black hole embedded in Friedmann spacetimes.
