359 research outputs found
Phase Transitions and Critical Behavior for Charged Black Holes
We investigate the thermodynamics of a four-dimensional charged black hole in
a finite cavity in asymptotically flat and asymptotically de Sitter space. In
each case, we find a Hawking-Page-like phase transition between a black hole
and a thermal gas very much like the known transition in asymptotically anti-de
Sitter space. For a ``supercooled'' black hole--a thermodynamically unstable
black hole below the critical temperature for the Hawking-Page phase
transition--the phase diagram has a line of first-order phase transitions that
terminates in a second order point. For the asymptotically flat case, we
calculate the critical exponents at the second order phase transition and find
that they exactly match the known results for a charged black hole in anti-de
Sitter space. We find strong evidence for similar phase transitions for the de
Sitter black hole as well. Thus many of the thermodynamic features of charged
anti-de Sitter black holes do not really depend on asymptotically anti-de
Sitter boundary conditions; the thermodynamics of charged black holes is
surprisingly universal.Comment: LaTeX, 14 pages, 9 eps figures; higher resolution figures available
on reques
Chaplygin Gas Cosmology - Unification of Dark Matter and Dark Energy
The models that unify dark matter and dark energy based upon the Chaplygin
gas fail owing to the suppression of structure formation by the adiabatic speed
of sound. Including string theory effects, in particular the Kalb-Ramond field,
we show how nonadiabatic perturbations allow a successful structure formation.Comment: 7 pages, presented by N. B. at IRGAC 2006, Barcelona, 11-15 July
2006, typos corrected, concluding paragraph slightly expanded, final version,
accepted in J. Phys. A, special issu
Hybrid Chaplygin gas and phantom divide crossing
Hybrid Chaplygin gas model is put forward, in which the gases play the role
of dark energy. For this model the coincidence problem is greatly alleviated.
The effective equation of state of the dark energy may cross the phantom divide
. Furthermore, the crossing behaviour is decoupled from any gravity
theories. In the present model, is only a transient behaviour. There is
a de Sitter attractor in the future infinity. Hence, the big rip singularity,
which often afflicts the models with matter whose effective equation of state
less than -1, is naturally disappear. There exist stable scaling solutions,
both at the early universe and the late universe. We discuss the perturbation
growth of this model. We find that the index is consistent with observations.Comment: 11 pages, 4 figures, V3: discussions on the perturbation growth
added, V4: minor corrections, to match the published versio
The Impact of Treated Urban Wastewaters and Flood Discharge on the Quality of Bathing Water
What do we know about the Adriatic Sea and the state of its health [...
Classification of dark energy models in the (w_0,w_a) plane
We classify dark energy models in a plane of observables that correspond to
the common parameterization of a non-constant equation of state, w(a)=w_0 +
w_a(1-a), where is the scale factor of the universe. The models fall into
four classes and only two of these classes have a region of overlap in the
observable plane. We perform a joint analysis of all Type Ia supernova (SNIa)
data compiled by the High-Z SN Search Team (HZT) and the Supernova Legacy
Survey (SNLS) and find that no class of models is excluded by current SNIa
data. However, an analysis of large scale structure, Ly forest and bias
constraints from SDSS, the Gold SNIa data and WMAP data indicates that
non-phantom barotropic models with a a positive sound speed are excluded at the
95% C.L.Comment: 11 pages, 3 figures. Classification generalized to include models for
which the equation of state crosses the phantom divide line. Published
versio
Tachyon cosmology with non-vanishing minimum potential: a unified model
We investigate the tachyon condensation process in the effective theory with
non-vanishing minimum potential and its implications to cosmology. It is shown
that the tachyon condensation on an unstable three-brane described by this
modified tachyon field theory leads to lower-dimensional branes (defects)
forming within a stable three-brane. Thus, in the cosmological background, we
can get well-behaved tachyon matter after tachyon inflation, (partially)
avoiding difficulties encountered in the original tachyon cosmological models.
This feature also implies that the tachyon inflated and reheated universe is
followed by a Chaplygin gas dark matter and dark energy universe. Hence, such
an unstable three-brane behaves quite like our universe, reproducing the key
features of the whole evolutionary history of the universe and providing a
unified description of inflaton, dark matter and dark energy in a very simple
single-scalar field model.Comment: 18 p
Fermion determinants in matrix models of QCD at nonzero chemical potential
The presence of a chemical potential completely changes the analytical
structure of the QCD partition function. In particular, the eigenvalues of the
Dirac operator are distributed over a finite area in the complex plane, whereas
the zeros of the partition function in the complex mass plane remain on a
curve. In this paper we study the effects of the fermion determinant at nonzero
chemical potential on the Dirac spectrum by means of the resolvent, G(z), of
the QCD Dirac operator. The resolvent is studied both in a one-dimensional U(1)
model (Gibbs model) and in a random matrix model with the global symmetries of
the QCD partition function. In both cases we find that, if the argument z of
the resolvent is not equal to the mass m in the fermion determinant, the
resolvent diverges in the thermodynamic limit. However, for z =m the resolvent
in both models is well defined. In particular, the nature of the limit is illuminated in the Gibbs model. The phase structure of the
random matrix model in the complex m and \mu-planes is investigated both by a
saddle point approximation and via the distribution of Yang-Lee zeros. Both
methods are in complete agreement and lead to a well-defined chiral condensate
and quark number density.Comment: 27 pages, 6 figures, Late
Phase transitions in self-gravitating systems. Self-gravitating fermions and hard spheres models
We discuss the nature of phase transitions in self-gravitating systems both
in the microcanonical and in the canonical ensemble. We avoid the divergence of
the gravitational potential at short distances by considering the case of
self-gravitating fermions and hard spheres models. Three kinds of phase
transitions (of zeroth, first and second order) are evidenced. They separate a
``gaseous'' phase with a smoothly varying distribution of matter from a
``condensed'' phase with a core-halo structure. We propose a simple analytical
model to describe these phase transitions. We determine the value of energy (in
the microcanonical ensemble) and temperature (in the canonical ensemble) at the
transition point and we study their dependance with the degeneracy parameter
(for fermions) or with the size of the particles (for a hard spheres gas).
Scaling laws are obtained analytically in the asymptotic limit of a small short
distance cut-off. Our analytical model captures the essential physics of the
problem and compares remarkably well with the full numerical solutions.Comment: Submitted to Phys. Rev. E. New material adde
Stable gravastars with generalised exteriors
New spherically symmetric gravastar solutions, stable to radial
perturbations, are found by utilising the construction of Visser and Wiltshire.
The solutions possess an anti--de Sitter or de Sitter interior and a
Schwarzschild--(anti)--de Sitter or Reissner--Nordstr\"{o}m exterior. We find a
wide range of parameters which allow stable gravastar solutions, and present
the different qualitative behaviours of the equation of state for these
parameters.Comment: 14 pages, 11 figures, to appear in Classical and Quantum Gravit
Gravastars must have anisotropic pressures
One of the very small number of serious alternatives to the usual concept of
an astrophysical black hole is the "gravastar" model developed by Mazur and
Mottola; and a related phase-transition model due to Laughlin et al. We
consider a generalized class of similar models that exhibit continuous pressure
-- without the presence of infinitesimally thin shells. By considering the
usual TOV equation for static solutions with negative central pressure, we find
that gravastars cannot be perfect fluids -- anisotropic pressures in the
"crust" of a gravastar-like object are unavoidable. The anisotropic TOV
equation can then be used to bound the pressure anisotropy. The transverse
stresses that support a gravastar permit a higher compactness than is given by
the Buchdahl--Bondi bound for perfect fluid stars. Finally we comment on the
qualitative features of the equation of state that gravastar material must have
if it is to do the desired job of preventing horizon formation.Comment: V1: 15 pages; 4 figures; uses iopart.cls; V2: 16 pages; added 3
references and brief discussio
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