1,392 research outputs found
Stretching of the toroidal field and generation of magnetosonic waves in differentially rotating plasma
We evaluate the generation of magnetosonic waves in differentially rotating
magnetized plasma. Differential rotation leads to an increase of the azimuthal
field by winding up the poloidal field lines into the toroidal field lines. An
amplification of weak seed perturbations is considered in this time-dependent
background state. It is shown that seed perturbations can be amplified by
several orders of magnitude in a differentially rotating flow. The only
necessary condition for this amplification is the presence of a non-vanishing
component of the magnetic field in the direction of the angular velocity
gradient.Comment: 5 pages, 5 figure
The neutron star in Cassiopeia A: equation of state, superfluidity, and Joule heating
The thermomagnetic evolution of the young neutron star in Cassiopea A is
studied by considering fast neutrino emission processes. In particular, we
consider neutron star models obtained from the equation of state computed in
the framework of the Brueckner-Bethe-Goldstone many-body theory and variational
methods, and models obtained with the Akmal-Pandharipande-Ravenhall equation of
state. It is shown that it is possible to explain a fast cooling regime as the
one observed in the neutron star in Cassiopea A if the Joule heating produced
by dissipation of the small-scale magnetic field in the crust is taken into
account. We thus argue that it is difficult to put severe constraints on the
superfluid gap if the Joule heating is considered.Comment: 4 pages, 2 figures, to appear on A&A Letter
A Class of Renormalization Group Invariant Scalar Field Cosmologies
We present a class of scalar field cosmologies with a dynamically evolving
Newton parameter and cosmological term . In particular, we discuss
a class of solutions which are consistent with a renormalization group scaling
for and near a fixed point. Moreover, we propose a modified
action for gravity which includes the effective running of and
near the fixed point. A proper understanding of the associated variational
problem is obtained upon considering the four-dimensional gradient of the
Newton parameter.Comment: 10 pages, RevTex4, no figures, to appear on GR
Renormalization Group in Quantum Mechanics
We establish the renormalization group equation for the running action in the
context of a one quantum particle system. This equation is deduced by
integrating each fourier mode after the other in the path integral formalism.
It is free of the well known pathologies which appear in quantum field theory
due to the sharp cutoff. We show that for an arbitrary background path the
usual local form of the action is not preserved by the flow. To cure this
problem we consider a more general action than usual which is stable by the
renormalization group flow. It allows us to obtain a new consistent
renormalization group equation for the action.Comment: 20 page
Recurrence and algorithmic information
In this paper we initiate a somewhat detailed investigation of the
relationships between quantitative recurrence indicators and algorithmic
complexity of orbits in weakly chaotic dynamical systems. We mainly focus on
examples.Comment: 26 pages, no figure
Protoneutron star dynamos and pulsar magnetism
We have investigated the turbulent mean-field dynamo action in protoneutron
stars that are subject to convective and neutron finger instabilities during
the early evolutionary phase. While the first one develops mostly in the inner
regions of the star, the second one is favored in the outer regions, where the
Rossby number is much smaller and a mean-field dynamo action is more efficient.
By solving the mean-field induction equation we have computed the critical spin
period below which no dynamo action is possible and found it to be s
for a wide range of stellar models and for both axisymmetric and
non-axisymmetric magnetic fields. Because this critical period is substantially
longer than the characteristic spin period of very young pulsars, we expect
that a mean-field dynamo will be effective for most protoneutron stars. The
saturation dipole field estimated by making use of the model of ``global''
quenching fits well the pulsar magnetic fields inferred from the spin-down
data. Apart from the large scale magnetic field, our model predicts also a
generation of small scale fields which are typically stronger than the poloidal
field and can survive during the lifetime of pulsars. Extremely rapidly
rotating protoneutron stars ( ms) may have the dipole field G.Comment: 7 pages, 6 figures, to appear on A&
The Universe With Bulk Viscosity
Exact solutions for a model with variable , and bulk viscosity
are obtained. Inflationary solutions with constant (de Sitter-type) and
variable energy density are found. An expanding anisotropic universe is found
to isotropize during its course of expansion but a static universe is not. The
gravitational constant is found to increase with time and the cosmological
constant decreases with time as .Comment: 7 LateX pages, no figure
Comment on "Feynman Effective Classical Potential in the Schrodinger Formulation"
We comment on the paper "Feynman Effective Classical Potential in the
Schrodinger Formulation"[Phys. Rev. Lett. 81, 3303 (1998)]. We show that the
results in this paper about the time evolution of a wave packet in a double
well potential can be properly explained by resorting to a variational
principle for the effective action. A way to improve on these results is also
discussed.Comment: 1 page, 2eps figures, Revte
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