6,935 research outputs found
Quantum revivals and carpets in some exactly solvable systems
We consider the revival properties of quantum systems with an eigenspectrum
E_{n} proportional to n^{2}, and compare them with the simplest member of this
class - the infinite square well. In addition to having perfect revivals at
integer multiples of the revival time t_{R}, these systems all enjoy perfect
fractional revivals at quarterly intervals of t_{R}. A closer examination of
the quantum evolution is performed for the Poeschel-Teller and Rosen-Morse
potentials, and comparison is made with the infinite square well using quantum
carpets.Comment: 5 pages, 5 figures (1 new), minor additions, to appear in J. Phys.
Testing Scalar-Tensor Gravity Using Space Gravitational-Wave Interferometers
We calculate the bounds which could be placed on scalar-tensor theories of
gravity of the Jordan, Fierz, Brans and Dicke type by measurements of
gravitational waveforms from neutron stars (NS) spiralling into massive black
holes (MBH) using LISA, the proposed space laser interferometric observatory.
Such observations may yield significantly more stringent bounds on the
Brans-Dicke coupling parameter \omega than are achievable from solar system or
binary pulsar measurements. For NS-MBH inspirals, dipole gravitational
radiation modifies the inspiral and generates an additional contribution to the
phase evolution of the emitted gravitational waveform. Bounds on \omega can
therefore be found by using the technique of matched filtering. We compute the
Fisher information matrix for a waveform accurate to second post-Newtonian
order, including the effect of dipole radiation, filtered using a currently
modeled noise curve for LISA, and determine the bounds on \omega for several
different NS-MBH canonical systems. For example, observations of a 1.4 solar
mass NS inspiralling to a 1000 solar mass MBH with a signal-to-noise ratio of
10 could yield a bound of \omega > 240,000, substantially greater than the
current experimental bound of \omega > 3000.Comment: 18 pages, 4 figures, 1 table; to be submitted to Phys. Rev.
Post-Newtonian gravitational radiation and equations of motion via direct integration of the relaxed Einstein equations. V. Evidence for the strong equivalence principle to second post-Newtonian order
Using post-Newtonian equations of motion for fluid bodies valid to the second
post-Newtonian order, we derive the equations of motion for binary systems with
finite-sized, non-spinning but arbitrarily shaped bodies. In particular we
study the contributions of the internal structure of the bodies (such as
self-gravity) that would diverge if the size of the bodies were to shrink to
zero. Using a set of virial relations accurate to the first post-Newtonian
order that reflect the stationarity of each body, and redefining the masses to
include 1PN and 2PN self-gravity terms, we demonstrate the complete
cancellation of a class of potentially divergent, structure-dependent terms
that scale as s^{-1} and s^{-5/2}, where s is the characteristic size of the
bodies. This is further evidence of the Strong Equivalence Principle, and
supports the use of post-Newtonian approximations to derive equations of motion
for strong-field bodies such as neutron stars and black holes. This extends
earlier work done by Kopeikin.Comment: 14 pages, submitted to Phys. Rev. D; small changes to coincide with
published versio
Revisiting the double-binary-pulsar probe of non-dynamical Chern-Simons gravity
One of the popular modifications to the theory of general relativity is
non-dynamical Chern-Simons (CS) gravity, in which the metric is coupled to an
externally prescribed scalar field. Setting accurate constraints to the
parameters of the theory is important owing to their implications for the
scalar field and/or the underlying fundamental theory. The current best
constraints rely on measurements of the periastron precession rate in the
double-binary-pulsar system and place a very tight bound on the characteristic
CS lengthscale k_cs^{-1} <~ 3*10^{-9} km. This paper considers several effects
that were not accounted for when deriving this bound and lead to a substantial
suppression of the predicted rate of periastron precession. It is shown, in
particular, that the point mass approximation for extended test bodies does not
apply in this case. The constraint to the characteristic CS lengthscale is
revised to k_cs^{-1} <~ 0.4 km, eight orders of magnitude weaker than what was
previously found.Comment: 12 pages, 4 figures, to be submitted to PRD. Comments are welcom
Cerenkov's Effect and Neutrino Oscillations in Loop Quantum Gravity
Bounds on the scale parameter {\cal L} arising in loop quantum gravity theory
are derived in the framework of Cerenkov's effect and neutrino oscillations.
Assuming that {\cal L} is an universal constant, we infer {\cal L}>
10^{-18}eV^{-1}, a bound compatible with ones inferred in different physical
context.Comment: 6 pages, no figures, in print on MPL
Solar irradiance models and measurements: a comparison in the 220 nm to 240 nm wavelength band
Solar irradiance models that assume solar irradiance variations to be due to
changes in the solar surface magnetic flux have been successfully used to
reconstruct total solar irradiance on rotational as well as cyclical and
secular time scales. Modelling spectral solar irradiance is not yet as
advanced, and also suffers from a lack of comparison data, in particular on
solar-cycle time scales. Here we compare solar irradiance in the 220 nm to 240
nm band as modelled with SATIRE-S and measured by different instruments on the
UARS and SORCE satellites.
We find good agreement between the model and measurements on rotational time
scales. The long-term trends, however, show significant differences. Both SORCE
instruments, in particular, show a much steeper gradient over the decaying part
of cycle 23 than the modelled irradiance or that measured by UARS/SUSIM.Comment: 8 pages, 2 figures, conference proceedings to appear in Surveys in
Geophysic
Love Me Lots And Love Me All The Time : Song
https://digitalcommons.library.umaine.edu/mmb-vp/5800/thumbnail.jp
Probing the Brans-Dicke Gravitational Field by Cerenkov Radiation
The possibility that a charged particle propagating in a gravitational field
described by Brans-Dicke theory of gravity could emit Cerenkov radiation is
explored. This process is kinematically allowed depending on parameters
occurring in the theory. The Cerenkov effect disappears as the BD parameter
omega tends to inftinity, i.e. in the limit in which the Einstein theory is
recovered, giving a signature to probe the validity of the Brans-Dicke theory.Comment: 8 pages, no figure
Variational Integrators for the Gravitational N-Body Problem
This paper describes a fourth-order integration algorithm for the
gravitational N-body problem based on discrete Lagrangian mechanics. When used
with shared timesteps, the algorithm is momentum conserving and symplectic. We
generalize the algorithm to handle individual time steps; this introduces
fifth-order errors in angular momentum conservation and symplecticity. We show
that using adaptive block power of two timesteps does not increase the error in
symplecticity. In contrast to other high-order, symplectic, individual
timestep, momentum-preserving algorithms, the algorithm takes only forward
timesteps. We compare a code integrating an N-body system using the algorithm
with a direct-summation force calculation to standard stellar cluster
simulation codes. We find that our algorithm has about 1.5 orders of magnitude
better symplecticity and momentum conservation errors than standard algorithms
for equivalent numbers of force evaluations and equivalent energy conservation
errors.Comment: 31 pages, 8 figures. v2: Revised individual-timestepping description,
expanded comparison with other methods, corrected error in predictor
equation. ApJ, in pres
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