561 research outputs found
On the linear and weak-field limits of scalar-tensor theories of gravity
The linear approximation of scalar-tensor theories of gravity is obtained in
the physical (Jordan) frame under the 4+0 (covariant) and 3+1 formalisms. Then
the weak-field limit is analyzed and the conditions leading to significant
deviations of the Newton's law of gravitation are discussed. Finally,
the scalarization effects induced by these theories in extended objects are
confronted within the weak-field limit.Comment: 12 pages in revtex4-twocolumn format; submitted to Phys.Rev.
Obstructions towards a generalization of no-hair theorems: I. Scalar clouds around Kerr black holes
We show that the integral method used to prove the no-hair theorem for Black
Holes (BH's) in spherically symmetric and static spacetimes within the
framework of general relativity with matter composed by a complex-valued
scalar-field does not lead to a straightforward conclusion about the absence of
hair in the stationary and rotating (axisymmetric) scenario. We argue that such
a failure can be used to justify in a simple and heuristic way the existence of
non-trivial boson clouds or hair found numerically by Herdeiro and Radu [1,2]
and analytically by Hod in the test field limit [3-5]. This is due to the
presence of a contribution that is negative when rotation exists which allows
for an integral to vanish even when a non-trivial boson hair is present. The
presence of such a negative contribution that depends on the rotation
properties of the BH is perfectly correlated with the eigenvalue problem
associated with the boson-field equation. Conversely, when the rotation is
absent the integral turns to be composed only by non negative (i.e. positive
semidefinite) terms and thus the only way it can vanish is when the hair is
completely absent. This analysis poses serious challenges and obstructions
towards the elaboration of no-hair theorems for more general spacetimes endowed
with a BH region even when including matter fields that obey the energy
conditions. Thus rotating boson stars, if collapsed, may lead indeed to a new
type of rotating BH, like the ones found in [1,2]. In order to achieve this
analysis we solve numerically the eigenvalue problem for the boson field in the
Kerr-BH background by imposing rigorous regularity conditions at the BH horizon
for the non-extremal case () which include the near extremal one in the
limit , as well as the small BH limit .Comment: 17 pages, 9 figures, 4 table
Cosmic acceleration in asymptotically Ricci flat Universe
We analyze the evolution of a Friedmann-Robertson-Walker spacetime within the
framework of metric gravity using an exponential model. We show that
gravity may lead to a vanishing effective cosmological constant in the
far future (i.e. ) and yet produce a transient accelerated
expansion at present time with a potentially viable cosmological history. This
is in contrast with several models which, while viable, produce in
general a non-vanishing effective cosmological constant asymptotically in time
(). We also show that relativistic {stars in
asymptotically flat spacetimes can be supported within this framework without
encountering any singularity, notably in the Ricci scalar .Comment: 12 pages, 18 figures in 9 panel
Has cosmological dark matter been observed?
There are many indications that ordinary matter represents only a tiny
fraction of the matter content of the Universe, with the remainder assumed to
consist of some different type of matter, which, for various reasons must be
nonluminous (dark matter). Among these indications are the inflationary
scenarios which predicts that the average energy density of the Universe
coincides with the so called critical value (for which the expansion never
stops but the rate of expansion approaches zero at very late times). At the
same time it is known (from the predictions of Big Bang nucleosynthesis on the
abundances of the light elements, other than Helium) that the baryonic energy
density (ordinary matter) must represent ( \% (where is
the Hubble constant in units of 100 km sMpc) of this critical
value \cite{Copi,OstStein}. We present here evidence supporting the model in
which the rest of the energy density corresponds to a scalar field, which can
be observed, however indirectly, in the oscillation of the effective
gravitational constant, and manifests itself in the known periodicity of the
number distribution of galaxies \cite{Broad,Szalay}. We analyze this model
numerically and show that, the requirement that the model satisfy the bounds of
light element abundances in the Universe, as predicted by Big Bang
nucleosynthesis, yields a specific value for the red-shift-galactic-count
oscillation amplitude compatible with that required to explain the oscillations
described above \cite{hill,CritStein}, and, furthermore, yields a value for the
age of the Universe compatible with standard bounds \cite{OstStein}.Comment: Latex file 15 pages with no figures. Please contact M.Salgado for
figures. This paper was submitted the 4 June as a letter for publication in
Natur
Cosmology in f(R) exponential gravity
Using an approach that treats the Ricci scalar itself as a degree of freedom,
we analyze the cosmological evolution within an f(R) model that has been
proposed recently (exponential gravity) and that can be viable for explaining
the accelerated expansion and other features of the Universe. This approach
differs from the usual scalar-tensor method and, among other things, it spares
us from dealing with unnecessary discussions about frames. It also leads to a
simple system of equations which is particularly suited for a numerical
analysis.Comment: 8 pages (no page numbers), 5 figures (10 panels). Prepared for the
Proceedings of Relativity and Gravitation: 100 years after Einstein in
Prague, Prague, 25-29 June, 201
Scalar hairy black holes and scalarons in the isolated horizons formalism
The Isolated Horizons (IH) formalism, together with a simple phenomenological
model for colored black holes has been used to predict non-trivial formulae
that relate the ADM mass of the solitons and hairy Black Holes of
Gravity-Matter system on the one hand, and several horizon properties of the
black holes in the other. In this article, the IH formalism is tested
numerically for spherically symmetric solutions to an Einstein-Higgs system
where hairy black holes were recently found to exist. It is shown that the mass
formulae still hold and that, by appropriately extending the current model, one
can account for the behavior of the horizon properties of these new solutions.
An empirical formula that approximates the ADM mass of hairy solutions is put
forward, and some of its properties are analyzed.Comment: 17 pages, 10 figures; revtex style; figures added; text updated to
match the published pape
The initial value problem of scalar-tensor theories of gravity
The initial value problem of scalar-tensor theories of gravity (STT) is
analyzed in the physical (Jordan) frame using a 3+1 decomposition of spacetime.
A first order strongly hyperbolic system is obtained for which the well
posedness of the Cauchy problem can be established. We provide two simple
applications of the 3+1 system of equations: one for static and spherically
symmetric spacetimes which allows the construction of unstable initial data
(compact objects) for which a further black hole formation and scalar
gravitational wave emission can be analyzed, and another application is for
homogeneous and isotropic spacetimes that permits to study the dynamics of the
Universe in the framework of STT.Comment: 12 pages; RevTex; Published in the Proceedings of the VII Mexican
School on Gravitation and Mathematical Physic
About matter and dark-energy domination eras in R^n gravity or lack thereof
We provide further numerical evidence which shows that R^n models in f(R)
metric gravity whether produces a late time acceleration in the Universe or a
matter domination era (usually a transient one) but not both. Our results
confirm the findings of Amendola et al. (2007), but using a different approach
that avoids the mapping to scalar-tensor theories of gravity, and therefore,
dispense us from any discussion or debate about frames (Einstein vs Jordan)
which are endemic in this subject. This class of models has been used
extensively in the literature as an alternative to the dark energy, but should
be considered ruled out for being inconsistent with observations. Finally, we
discuss a caveat in the analysis by Faraoni (2011), which was used to further
constrain these models by using a chameleon mechanism.Comment: 6 pages, 6 figures in 2 panels. Accepted for publication in Phys.
Rev.
The Einstein-Maxwell system in 3+1 form and initial data for multiple charged black holes
We consider the Einstein-Maxwell system as a Cauchy initial value problem
taking the electric and magnetic fields as independent variables. Maxwell's
equations in curved spacetimes are derived in detail using a 3+1 formalism and
their hyperbolic properties are analyzed, showing that the resulting system is
symmetric hyperbolic. We also focus on the problem of finding initial data for
multiple charged black holes assuming time-symmetric initial data and using a
puncture-like method to solve the Hamiltonian and the Gauss constraints. We
study the behavior of the resulting initial data families, and show that
previous results in this direction can be obtained as particular cases of our
approach.Comment: 20 pages, 6 figures, some typos fixed and references adde
f(R) Cosmology revisited
We consider a class of metric f(R) modified gravity theories, analyze them in
the context of a Friedmann-Robertson-Walker cosmology and confront the results
with some of the known constraints imposed by observations. In particular, we
focus in correctly reproducing the matter and effective cosmological constant
eras, the age of the Universe, and supernovae data. Our analysis differs in
many respects from previous studies. First, we avoid any transformation to a
scalar-tensor theory in order to be exempted of any potential pathologies (e.g.
multivalued scalar potentials) and also to evade any unnecessary discussion
regarding frames (i.e. Einstein vs Jordan). Second, based on a robust approach,
we recast the cosmology equations as an initial value problem subject to a
modified Hamiltonian constraint. Third, we solve the equations numerically
where the Ricci scalar itself is one of the variables, and use the constraint
equation to monitor the accuracy of the solutions. We compute the "equation of
state" (EOS) associated with the modifications of gravity using several
inequivalent definitions that have been proposed in the past and analyze it in
detail. We argue that one of these definitions has the best features. In
particular, we present the EOS around the so called "phantom divide" boundary
and compare it with previous findings.Comment: 35 pages; 33 figures; revte
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