21,912 research outputs found
Dark energy: a quantum fossil from the inflationary Universe?
The discovery of dark energy (DE) as the physical cause for the accelerated
expansion of the Universe is the most remarkable experimental finding of modern
cosmology. However, it leads to insurmountable theoretical difficulties from
the point of view of fundamental physics. Inflation, on the other hand,
constitutes another crucial ingredient, which seems necessary to solve other
cosmological conundrums and provides the primeval quantum seeds for structure
formation. One may wonder if there is any deep relationship between these two
paradigms. In this work, we suggest that the existence of the DE in the present
Universe could be linked to the quantum field theoretical mechanism that may
have triggered primordial inflation in the early Universe. This mechanism,
based on quantum conformal symmetry, induces a logarithmic,
asymptotically-free, running of the gravitational coupling. If this evolution
persists in the present Universe, and if matter is conserved, the general
covariance of Einstein's equations demands the existence of dynamical DE in the
form of a running cosmological term whose variation follows a power law of the
redshift.Comment: LaTeX, 14 pages, extended discussion. References added. Accepted in
J. Phys. A: Mathematical and Theoretica
Next to leading order non Fermi liquid corrections to the neutrino emissivity and cooling of the neutron star
In this work we derive the expressions of the neutrino mean free path(MFP)
and emissivity with non Fermi liquid corrections up to next to leading
order(NLO) in degenerate quark matter. The calculation has been performed both
for the absorption and scattering processes. Subsequently the role of these NLO
corrections on the cooling of the neutron star has been demonstrated. The
cooling curve shows moderate enhancement compared to the leading order(LO)
non-Fermi liquid result. Although the overall correction to the MFP and
emissivity are larger compared to the free Fermi gas, the cooling behavior does
not alter significantly.Comment: 8 pages, 8 figures, references added, matches published versio
Non-rotating and rotating neutron stars in the extended field theoretical model
We study the properties of non-rotating and rotating neutron stars for a new
set of equations of state (EOSs) with different high density behaviour obtained
using the extended field theoretical model. The high density behaviour for
these EOSs are varied by varying the meson self-coupling and
hyperon-meson couplings in such a way that the quality of fit to the bulk
nuclear observables, nuclear matter incompressibility coefficient and
hyperon-nucleon potential depths remain practically unaffected. We find that
the largest value for maximum mass for the non-rotating neutron star is
. The radius for the neutron star with canonical mass is km provided only those EOSs are considered for which maximum mass is
larger than as it is the lower bound on the maximum mass measured
so far. Our results for the very recently discovered fastest rotating neutron
star indicate that this star is supra massive with mass and
circumferential equatorial radius km.Comment: 28 pages, 12 figures. Phys. Rev. C (in press
Cosmology with variable parameters and effective equation of state for Dark Energy
A cosmological constant, Lambda, is the most natural candidate to explain the
origin of the dark energy (DE) component in the Universe. However, due to
experimental evidence that the equation of state (EOS) of the DE could be
evolving with time/redshift (including the possibility that it might behave
phantom-like near our time) has led theorists to emphasize that there might be
a dynamical field (or some suitable combination of them) that could explain the
behavior of the DE. While this is of course one possibility, here we show that
there is no imperative need to invoke such dynamical fields and that a variable
cosmological constant (including perhaps a variable Newton's constant too) may
account in a natural way for all these features.Comment: LaTeX, 9 pages, 1 figure. Talk given at the 7th Intern. Workshop on
Quantum Field Theory Under the Influence of External Conditions (QFEXT 05
Medium effects of magnetic moments of baryons on neutron stars under strong magnetic fields
We investigate medium effects due to density-dependent magnetic moments of
baryons on neutron stars under strong magnetic fields. If we allow the
variation of anomalous magnetic moments (AMMs) of baryons in dense matter under
strong magnetic fields, AMMs of nucleons are enhanced to be larger than those
of hyperons. The enhancement naturally affects the chemical potentials of
baryons to be large and leads to the increase of a proton fraction.
Consequently, it causes the suppression of hyperons, resulting in the stiffness
of the equation of state. Under the presumed strong magnetic fields, we
evaluate relevant particles' population, the equation of state and the maximum
masses of neutron stars by including density-dependent AMMs and compare them
with those obtained from AMMs in free space
Correlations in the properties of static and rapidly rotating compact stars
Correlations in the properties of the static compact stars (CSs) and the ones
rotating with the highest observed frequency of 1122Hz are studied using a
large set of equations of state (EOSs). These EOSs span various approaches and
their chemical composition vary from the nucleons to hyperons and quarks in
-equilibrium. It is found that the properties of static CS, like, the
maximum gravitational mass and radius corresponding to t he canonical mass and supramassive or
non-supramassive nature of the CS rotating at 1122 Hz are strongly correlated.
In particular, only those EOSs yield the CS rotating at 1122Hz to be
non-supramassive for which \left (\frac{M_{\rm max}^{\rm stat}}{M_\odot}\right
)^{1/2} \left (\frac{10{\rm km}}{R_{1.4}^{\rm stat}})^{3/2} is greater than
unity. Suitable parametric form which can be used to split the plane into the regions of different
supramassive nature of the CS rotating at 1122Hz is presented. Currently
measured maximum gravitational mass 1.76 of PSR J0437-4715 suggests
that the CS rotating at 1122Hz can be non-supramassive provided km.Comment: 13 pages, 4 figures, Appearing in Phys. Rev.
A SuperMassive Black Hole Fundamental Plane for Ellipticals
We obtain the coefficients of a new fundamental plane for supermassive black
holes at the centers of elliptical galaxies, involving measured central black
hole mass and photometric parameters which define the light distribution. The
galaxies are tightly distributed around this mass fundamental plane, with
improvement in the rms residual over those obtained from the \mbh-\sigma and
\mbh-L relations. This implies a strong multidimensional link between the
central massive black hole formation and global photometric properties of
elliptical galaxies and provides an improved estimate of black hole mass from
galaxy data.Comment: Accepted for publication in ApJ Letter
The nature of solar brightness variations
The solar brightness varies on timescales from minutes to decades.
Determining the sources of such variations, often referred to as solar noise,
is of importance for multiple reasons: a) it is the background that limits the
detection of solar oscillations, b) variability in solar brightness is one of
the drivers of the Earth's climate system, c) it is a prototype of stellar
variability which is an important limiting factor for the detection of
extra-solar planets. Here we show that recent progress in simulations and
observations of the Sun makes it finally possible to pinpoint the source of the
solar noise. We utilise high-cadence observations from the Solar Dynamic
Observatory and the SATIRE model to calculate the magnetically-driven
variations of solar brightness. The brightness variations caused by the
constantly evolving cellular granulation pattern on the solar surface are
computed with the MURAM code. We find that surface magnetic field and
granulation can together precisely explain solar noise on timescales from
minutes to decades, i.e. ranging over more than six orders of magnitude in the
period. This accounts for all timescales that have so far been resolved or
covered by irradiance measurements. We demonstrate that no other sources of
variability are required to explain the data. Recent measurements of Sun-like
stars by CoRoT and Kepler uncovered brightness variations similar to that of
the Sun but with much wider variety of patterns. Our finding that solar
brightness variations can be replicated in detail with just two well-known
sources will greatly simplify future modelling of existing CoRoT and Kepler as
well as anticipated TESS and PLATO data.Comment: This is the submitted version of the paper published in Nature
Astronom
Gravitational Wavetrains in the Quasi-Equilibrium Approximation: A Model Problem in Scalar Gravitation
A quasi-equilibrium (QE) computational scheme was recently developed in
general relativity to calculate the complete gravitational wavetrain emitted
during the inspiral phase of compact binaries. The QE method exploits the fact
that the the gravitational radiation inspiral timescale is much longer than the
orbital period everywhere outside the ISCO. Here we demonstrate the validity
and advantages of the QE scheme by solving a model problem in relativistic
scalar gravitation theory. By adopting scalar gravitation, we are able to
numerically track without approximation the damping of a simple, quasi-periodic
radiating system (an oscillating spherical matter shell) to final equilibrium,
and then use the exact numerical results to calibrate the QE approximation
method. In particular, we calculate the emitted gravitational wavetrain three
different ways: by integrating the exact coupled dynamical field and matter
equations, by using the scalar-wave monopole approximation formula
(corresponding to the quadrupole formula in general relativity), and by
adopting the QE scheme. We find that the monopole formula works well for weak
field cases, but fails when the fields become even moderately strong. By
contrast, the QE scheme remains quite reliable for moderately strong fields,
and begins to breakdown only for ultra-strong fields. The QE scheme thus
provides a promising technique to construct the complete wavetrain from binary
inspiral outside the ISCO, where the gravitational fields are strong, but where
the computational resources required to follow the system for more than a few
orbits by direct numerical integration of the exact equations are prohibitive.Comment: 15 pages, 14 figure
Warm and dense stellar matter under strong magnetic fields
We investigate the effects of strong magnetic fields on the equation of state
of warm stellar matter as it may occur in a protoneutron star. Both neutrino
free and neutrino trapped matter at a fixed entropy per baryon are analyzed. A
relativistic mean field nuclear model, including the possibility of hyperon
formation, is considered. A density dependent magnetic field with the magnitude
G at the surface and not more than G at the center
is considered. The magnetic field gives rise to a neutrino suppression, mainly
at low densities, in matter with trapped neutrinos. It is shown that an hybrid
protoneutron star will not evolve to a low mass blackhole if the magnetic field
is strong enough and the magnetic field does not decay. However, the decay of
the magnetic field after cooling may give rise to the formation of a low mass
blackhole.Comment: 17 pages, 10 figures, 3 tables, submitted to Phys. Rev.
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