191 research outputs found
Prospects for gravitational-wave observations of neutron-star tidal disruption in neutron-star/black-hole binaries
For an inspiraling neutron-star/black-hole binary (NS/BH), we estimate the
gravity-wave frequency f_td at the onset of NS tidal disruption. We model the
NS as a tidally distorted, homogeneous, Newtonian ellipsoid on a circular,
equatorial geodesic around a Kerr BH. We find that f_td depends strongly on the
NS radius R, and estimate that LIGO-II (ca. 2006-2008) might measure R to 15%
precision at 140 Mpc (about 1 event/yr under current estimates). This suggests
that LIGO-II might extract valuable information about the NS equation of state
from tidal-disruption waves.Comment: RevTeX, 4 pages, 2 EPS figures. Revised slightly, corrected typo
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Routine inspection effort required for verification of a nuclear material production cutoff convention
Preliminary estimates of the inspection effort to verify a Nuclear Material Cutoff Convention are presented. The estimates are based on (1) a database of about 650 facilities a total of eight states, i.e., the five nuclear-weapons states and three ``threshold`` states; (2) typical figures for inspection requirements for specific facility types derived from IAEA experience, where applicable; and (3) alternative estimates of inspection effort in cutoff options where full IAEA safeguards are not stipulated. Considerable uncertainty must be attached to the effort estimates. About 50--60% of the effort for each option is attributable to 16 large-scale reprocessing plants assumed to be in operation in the eight states; it is likely that some of these will be shut down by the time the convention enters into force. Another important question involving about one third of the overall effort is whether Euratom inspections in France and the U.K. could obviate the need for full-scale IAEA inspections at these facilities. Finally, the database does not yet contain many small-scale and military-related facilities. The results are therefore not presented as predictions but as the consequences of alternative assumptions. Despite the preliminary nature of the estimates, it is clear that a broad application of NPT-like safeguards to the eight states would require dramatic increases in the IAEA`s safeguards budget. It is also clear that the major component of the increased inspection effort would occur at large reprocessing plants (and associated plutonium facilities). Therefore, significantly bounding the increased effort requires a limitation on the inspection effort in these facility types
Contact-limited currents in metal-insulator-metal structures
The physical mechanisms underlying current flow in solid-state MIM structures are reviewed with emphasis on criteria for determining the dominant conduction mechanism in a given experimental situation. Measurements of the bias and temperature dependence of currents through structures incorporating a thin film of single-crystal gallium selenide are reported, and are shown to be in excellent agreement with the predictions of a simple physical model of contact-limited emission. Independently measured properties of bulk single-crystal gallium selenide are used in all calculations; no adjustable parameters are employed. We believe that this study presents unequivocal evidence for contact-limited thermionic currents in solid-state MIM structures
Dynamics of thick discs around Schwarzschild-de Sitter black holes
We consider the effects of a cosmological constant on the dynamics of
constant angular momentum discs orbiting Schwarzschild-de Sitter black holes.
The motivation behind this study is to investigate whether the presence of a
radial force contrasting the black hole's gravitational attraction can
influence the occurrence of the runaway instability, a robust feature of the
dynamics of constant angular momentum tori in Schwarzschild and Kerr
spacetimes. In addition to the inner cusp near the black hole horizon through
which matter can accrete onto the black hole, in fact, a positive cosmological
constant introduces also an outer cusp through which matter can leave the torus
without accreting onto the black hole. To assess the impact of this outflow on
the development of the instability we have performed time-dependent and
axisymmetric hydrodynamical simulations of equilibrium initial configurations
in a sequence of background spacetimes of Schwarzschild-de Sitter black holes
with increasing masses. The simulations have been performed with an unrealistic
value for the cosmological constant which, however, yields sufficiently small
discs to be resolved accurately on numerical grids and thus provides a first
qualitative picture of the dynamics. The calculations, carried out for a wide
range of initial conditions, show that the mass-loss from the outer cusp can
have a considerable impact on the instability, with the latter being rapidly
suppressed if the outflow is large enough.Comment: 12 pages; A&A, in pres
An approximate binary-black-hole metric
An approximate solution to Einstein's equations representing two
widely-separated non-rotating black holes in a circular orbit is constructed by
matching a post-Newtonian metric to two perturbed Schwarzschild metrics. The
spacetime metric is presented in a single coordinate system valid up to the
apparent horizons of the black holes. This metric could be useful in numerical
simulations of binary black holes. Initial data extracted from this metric have
the advantages of being linked to the early inspiral phase of the binary
system, and of not containing spurious gravitational waves.Comment: 20 pages, 1 figure; some changes in Sec. IV B,C and Sec.
Magnetized Tori around Kerr Black Holes: Analytic Solutions with a Toroidal Magnetic Field
The dynamics of accretion discs around galactic and extragalactic black holes
may be influenced by their magnetic field. In this paper we generalise the
fully relativistic theory of stationary axisymmetric tori in Kerr metric of
Abramowicz et al.(1978) by including strong toroidal magnetic field and
construct analytic solutions for barotropic tori with constant angular
momentum. This development is particularly important for the general
relativistic computational magnetohydrodynamics that suffers from the lack of
exact analytic solutions that are needed to test computer codes.Comment: accepted for publication in MNRAS after substantial revision of the
section on simulation
Retarded coordinates based at a world line, and the motion of a small black hole in an external universe
In the first part of this article I present a system of retarded coordinates
based at an arbitrary world line of an arbitrary curved spacetime. The
retarded-time coordinate labels forward light cones that are centered on the
world line, the radial coordinate is an affine parameter on the null generators
of these light cones, and the angular coordinates are constant on each of these
generators. The spacetime metric in the retarded coordinates is displayed as an
expansion in powers of the radial coordinate and expressed in terms of the
world line's acceleration vector and the spacetime's Riemann tensor evaluated
at the world line. The formalism is illustrated in two examples, the first
involving a comoving world line of a spatially-flat cosmology, the other
featuring an observer in circular motion in the Schwarzschild spacetime. The
main application of the formalism is presented in the second part of the
article, in which I consider the motion of a small black hole in an empty
external universe. I use the retarded coordinates to construct the metric of
the small black hole perturbed by the tidal field of the external universe, and
the metric of the external universe perturbed by the presence of the black
hole. Matching these metrics produces the MiSaTaQuWa equations of motion for
the small black hole.Comment: 20 pages, revtex4, 2 figure
The runaway instability of thick discs around black holes. II. Non constant angular momentum discs
We present results from a comprehensive number of relativistic,
time-dependent, axisymmetric simulations of the runaway instability of
non-constant angular momentum thick discs around black holes. This second paper
extends earlier results where only constant angular momentum discs were
considered. All relevant aspects of the theory of stationary thick discs around
rotating black holes, necessary to build the initial state in our simulations,
are presented in great detail. The angular momentum of the discs is assumed to
increase outwards with the radial distance according to a power law. The main
simplifying assumptions of our approach are not to include magnetic fields and
self-gravity in the discs. Furthermore, the dynamics of the spacetime is
accounted for by computing the transfer of mass and angular momentum from the
disc to the black hole through the event horizon : the evolution of the central
black hole is assumed to follow a sequence of Kerr black holes of increasing
mass and spin. In agreement with previous results based on stationary models we
find that by allowing the mass and the spin of the black hole to grow, constant
angular momentum discs rapidly become unstable on a dynamical timescale. The
comparison with the results of paper I shows that the effect of the angular
momentum transfer from the torus to the black hole is to make constant angular
momentum discs less unstable, increasing the timescale of the instability.
However, we find that non-constant angular momentum discs are dramatically
stabilized for very small values of the angular momentum slope. Our
time-dependent simulations confirm, thus, the predictions of stationary studies
concerning the stabilizing effect of non-constant angular momentum
distributions.Comment: 36 pages, 18 figures, submitted to MNRA
On the Polish doughnut accretion disk via the effective potential approach
We revisit the Polish doughnut model of accretion disks providing a
comprehensive analytical description of the Polish doughnut structure. We
describe a perfect fluid circularly orbiting around a Schwarzschild black hole,
source of the gravitational field, by the effective potential approach for the
exact gravitational and centrifugal effects. This analysis leads to a detailed,
analytical description of the accretion disk, its toroidal surface, the
thickness, the distance from the source. We determine the variation of these
features with the effective potential and the fluid angular momentum. Many
analytical formulas are given. In particular it turns out that the distance
from the source of the inner surface of the torus increases with increasing
fluid angular momentum but decreases with increasing energy function defined as
the value of the effective potential for that momentum. The location of torus
maximum thickness moves towards the external regions of the surface with
increasing angular momentum, until it reaches a maximum an then decreases.
Assuming a polytropic equation of state we investigate some specific cases.Comment: 33 pages, 28 figures, 1 table. This is a revised version to meet the
published articl
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