A ug 2 00 8 A Better Way to Reconstruct Dark Energy Models ?

0 v 2 2 6 A ug 2 00 3 Cosmological constraints on a dark matter – dark energy interaction

It is generally assumed that the two dark components of the energy density of the universe, a smooth component called dark energy and a fluid of nonrelativistic weakly interacting particles called dark matter, are independent of each other and interact only through gravity. In this paper, we consider a class of models in which the dark matter and dark energy interact directly. The dark matter p...

ar X iv : 0 70 8 . 26 18 v 1 [ as tr o - ph ] 2 0 A ug 2 00 7 Using Local Volume data to constrain Dark Matter dynamics

ar X iv : 0 80 8 . 13 72 v 1 [ he p - ph ] 9 A ug 2 00

We investigate the minimal supergravity (mSUGRA) signals at the LHC in the context of supercritical string cosmology (SSC). In this theory, the presence of a time dependent dilaton provides us with a smoothly evolving dark energy and modifies the dark matter allowed region of the mSUGRA model with standard cosmology. Such a dilaton dilutes the supersymmetric dark matter density (of neutralinos)...

ar X iv : a st ro - p h / 02 08 13 8 v 1 7 A ug 2 00 2 Importance of Supernovae at z > 1 . 5 to Probe Dark Energy

The accelerating expansion of the universe suggests that an unknown component with strongly negative pressure, called dark energy, currently dominates the dynamics of the universe. Such a component makes up ∼ 70% of the energy density of the universe yet has not been predicted by the standard model of particle physics. The best method for exploring the nature of this dark energy is to map the r...

2 00 7 Interacting Holographic Phantom

In this paper we consider the holographic model of interacting dark energy in non-flat universe. With the choice of c ≤ 0.84, the interacting holographic dark energy can be described by a phantom scalar field. Then we show this phantomic description of the holographic dark energy with c ≤ 0.84 and reconstruct the potential of the phantom scalar field.