118428312
Energy conditions and stability in generalized f(R) gravity with arbitrary coupling between matter and geometry
Abstract The energy conditions and the Dolgov–Kawasaki criterion in generalized f ( R ) gravity with arbitrary coupling between matter and geometry are derived in this Letter, which are quite general and can degenerate to the well-known energy conditions in GR and f ( R ) gravity with non-minimal coupling and non-coupling as special cases. In order to get some insight on the meaning of these energy conditions and the Dolgov–Kawasaki criterion, we apply them to a class of models in the FRW cosmology and give some corresponding results.
122901072
INTERACTING GENERALIZED CHAPLYGIN GAS MODEL WITH HOLOGRAPHIC DARK ENERGY
In this paper we consider the interacting generalized Chaplygin gas model as a unified scheme, in which the holographic dark energy as the dark energy component interacts with the cold dark matter with wdm = 0. Concretely, we mainly discuss the two kinds of interactions between the dark energy and dark matter, and give the evolution trajectories of density parameter and equation of state of dark energy as well as the decelerate parameter. By analysis, we show that in both cases of Q = 3bHρde and Q = 3bHρGCG, the evolution laws and the present values of Ωde, wde and q are compatible with the astronomical observations, but the effects of the coupling constant and holographic constant on them are completely different.
118428312
Energy conditions and stability in generalized f(R) gravity with arbitrary coupling between matter and geometry
Abstract The energy conditions and the Dolgov–Kawasaki criterion in generalized f ( R ) gravity with arbitrary coupling between matter and geometry are derived in this Letter, which are quite general and can degenerate to the well-known energy conditions in GR and f ( R ) gravity with non-minimal coupling and non-coupling as special cases. In order to get some insight on the meaning of these energy conditions and the Dolgov–Kawasaki criterion, we apply them to a class of models in the FRW cosmology and give some corresponding results.
119262999
Extended Analysis on New Generalized Chaplygin Gas
We extend the study of the new generalized Chaplygin gas (NGCG) based on [J. Cosmol. Astropart. Phys. 0601 (2006) 003]. Specifically, we not only discuss the change rates of the energy densities and the energy transfer of this model, but also perform the Om diagnostic to differentiate the ΛCDM model from the NGCG and the GCG models. Furthermore, in order to consider the influence of dark energy on structure formation, we also present the evolution of the growth index in this scenario with interaction.
118610495
Conditions and instability in f(R) gravity with non-minimal coupling between matter and geometry
In this paper, on the basis of the generalized f(R) gravity model with arbitrary coupling between geometry and matter, four classes of f(R) gravity models with non-minimal coupling between geometry and matter will be studied. By means of conditions of power-law expansion and the equation of state of matter less than −1/3, the relationship among p, w and n, the conditions and the candidate for late-time cosmic accelerated expansion will be discussed in the four classes of f(R) gravity models with non-minimal coupling. Furthermore, in order to keep to considering models that are realistic ones, the Dolgov–Kawasaki instability will be investigated in each of them.
123724946
Expression of interest to the Superconducting Super Collider Laboratory by the L* Collaboration
199676084
Measurement of the differential q**2 spectrum and forward-backward asymmetry for B ---> K* l+ l-
6568600
No-go theorems for generalized chameleon field theories.
The chameleon, or generalizations thereof, is a light scalar that couples to matter with gravitational strength, but whose manifestation depends on the ambient matter density. A key feature is that the screening mechanism suppressing its effects in high-density environments is determined by the local scalar field value. Under very general conditions, we prove two theorems limiting its cosmological impact: (i) the Compton wavelength of such a scalar can be at most ~/= 1 MPc at the present cosmic density, which restricts its impact to nonlinear scales; and (ii) the conformal factor relating Einstein- and Jordan-frame scale factors is essentially constant over the last Hubble time, which precludes the possibility of self-acceleration. These results imply that chameleonlike scalar fields have a negligible effect on the linear-scale growth history; theories that invoke a chameleonlike scalar to explain cosmic acceleration rely on a form of dark energy rather than a genuine modified gravity effect. Our analysis applies to a broad class of chameleon, symmetron, and dilaton theories.
119533144
Excitation energy as a basic variable to control nuclear disassembly

Abstract: Thermodynamical features of Xe system is investigated as functions of temperature and freeze-out density in the frame of lattice gas model. The calculation shows different temperature dependence of physical observables at different freeze-out density. In this case, the critical temperature when the phase transition takes place depends on the freeze-out density. However, a unique critical excitation energy %and the same excitation reveals regardless of freeze-out density when the excitation energy is used as a variable instead of temperature. Moreover, the different behavior of other physical observables with temperature due to different ρf vanishes when excitation energy replaces temperature. It indicates that the excitation energy can be seen as a more basic quantity to control nuclear disassembly.
123480931
EFFECTIVE COSMOLOGICAL CONSTANT IN BRANE COSMOLOGY
We consider a brane-world of co-dimension one without reflection symmetry. Through it, we give a possible explanation of the great discrepancy between the vacuum energy and the observed cosmological constant without contradiction to the knowledge we have about our Universe. We also show the gravity observed will be standard four-dimensional gravity as long as the discrepancy of the bulk cosmological constant at different sides of the brane is small enough.