7,130 research outputs found
Stability of spherical stellar systems I : Analytical results
The so-called ``symplectic method'' is used for studying the linear stability
of a self-gravitating collisionless stellar system, in which the particles are
also submitted to an external potential. The system is steady and spherically
symmetric, and its distribution function thus depends only on the energy
and the squarred angular momentum of a particle. Assuming that
, it is first shown that stability holds with
respect to all the spherical perturbations -- a statement which turns out to be
also valid for a rotating spherical system. Thus it is proven that the energy
of an arbitrary aspherical perturbation associated to a ``preserving generator"
[i.e., one satisfying ] is always positive if and the
external mass density is a decreasing function of the distance to the
center. This implies in particular (under the latter condition) the stability
of an isotropic system with respect to all the perturbations. Some new remarks
on the relation between the symmetry of the system and the form of are
also reported. It is argued in particular that a system with a distribution
function of the form is necessarily spherically symmetric.Comment: uuencoded compressed postscript file containing 13 pages, accepted
for publication in MNRA
Wave Excitation in Disks Around Rotating Magnetic Stars
The accretion disk around a rotating magnetic star (neutron star, white dwarf
or T Tauri star) is subjected to periodic vertical magnetic forces from the
star, with the forcing frequency equal to the stellar spin frequency or twice
the spin frequency. This gives rise bending waves in the disk that may
influence the variabilities of the system. We study the excitation, propagation
and dissipation of these waves using a hydrodynamical model coupled with a
generic model description of the magnetic forces. The bending waves are
excited at the Lindblad/vertical resonance, and propagate either to larger
radii or inward toward the corotation resonance where dissipation takes place.
While the resonant torque is negligible compared to the accretion torque, the
wave nevertheless may reach appreciable amplitude and can cause or modulate
flux variabilities from the system. We discuss applications of our result to
the observed quasi-periodic oscillations from various systems, in particular
neutron star low-mass X-ray binaries.Comment: Small changes/clarifications. To be published in ApJ, Aug.20,2008
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Accretion disc-stellar magnetosphere interaction: field line inflation and the effect on the spin-down torque
We calculate the structure of a force-free magnetosphere which is assumed to
corotate with a central star and which interacts with an embedded
differentially rotating accretion disc. The magnetic and rotation axes are
aligned and the stellar field is assumed to be a dipole. We concentrate on the
case when the amount of field line twisting through the disc-magnetosphere
interaction is large and consider different outer boundary conditions. In
general the field line twisting produces field line inflation (eg. Bardou &
Heyvaerts 1996) and in some cases with large twisting many field lines can
become open. We calculate the spin-down torque acting between the star and the
disc and we find that it decreases significantly for cases with large field
line twisting. This suggests that the oscillating torques observed for some
accreting neutron stars could be due to the magnetosphere varying between
states with low and high field line inflation. Calculations of the spin
evolution of T Tauri stars may also have to be revised in light of the
significant effect that field line twisting has on the magnetic torque
resulting from star-disc interactions.Comment: Accepted by MNRAS. 21 pages, 15 figures. LaTeX2e in the MN style.
PostScript files are also available from http://www-star.qmw.ac.uk/~va/ or by
e-mail: [email protected]
Adapting Binary Information Retrieval Evaluation Metrics for Segment-based Retrieval Tasks
This report describes metrics for the evaluation of the effectiveness of
segment-based retrieval based on existing binary information retrieval metrics.
This metrics are described in the context of a task for the hyperlinking of
video segments. This evaluation approach re-uses existing evaluation measures
from the standard Cranfield evaluation paradigm. Our adaptation approach can in
principle be used with any kind of effectiveness measure that uses binary
relevance, and for other segment-baed retrieval tasks. In our video
hyperlinking setting, we use precision at a cut-off rank n and mean average
precision.Comment: Explanation of evaluation measures for the linking task of the
MediaEval Workshop 201
Systematic review and meta-analysis on outcomes of salvage therapy in patients with tumour recurrence during âwatch and waitâ in rectal cancer.
Introduction: The âwatch and waitâ approach has recently emerged as an alternative approach for managing patients with complete clinical response in rectal cancer. However, less is understood whether the intervention is associated with a favourable outcome among patients who require salvage therapy following local recurrence. Materials and methods: A comprehensive systematic search was performed using EMBASE, PubMed, MEDLINE, Journals@Ovid as well as hand searches; published between 2004 and 2018, to identify studies where outcomes of patients undergoing watch and wait were compared with conventional surgery. Study quality was assessed using the NewcastleâOttawa assessment scale. The main outcome was relative risks for overall and disease specific mortality in salvage therapy. Results: Nine eligible studies were included in the meta-analysis. Of 248 patients who followed the watch and wait strategy, 10.5% had salvage therapy for recurrent disease. No statistical heterogeneity was found in the results. The relative risk of overall mortality in the salvage therapy group was 2.42 (95% confidence interval 0.96â6.13) compared with the group who had conventional surgery, but this was not statistically significant (P > 0.05). The relative risk of disease specific mortality in salvage therapy was 2.63 (95% confidence interval 0.81â8.53). Conclusion: Our findings demonstrated that there was no significant difference in overall and disease specific mortality in patients who had salvage treatment following recurrence of disease in the watch and wait group compared with the standard treatment group. However, future research into the oncological safety of salvage treatment is needed
Microstructure-failure mode correlations in braided composites
Explication of the fracture processes of braided composites is needed for modeling their behavior. Described is a systematic exploration of the relationship between microstructure, loading mode, and micro-failure mechanisms in carbon/epoxy braided composites. The study involved compression and fracture toughness tests and optical and scanning electron fractography, including dynamic in-situ testing. Principal failure mechanisms of low sliding, buckling, and unstable crack growth are correlated to microstructural parameters and loading modes; these are used for defining those microstructural conditions which are strength limiting
Magnetically Torqued Thin Accretion Disks
We compute the properties of a geometrically thin, steady accretion disk
surrounding a central rotating, magnetized star. The magnetosphere is assumed
to entrain the disk over a wide range of radii. The model is simplified in that
we adopt two (alternate) ad hoc, but plausible, expressions for the azimuthal
component of the magnetic field as a function of radial distance. We find a
solution for the angular velocity profile tending to corotation close to the
central star, and smoothly matching a Keplerian curve at a radius where the
viscous stress vanishes. The value of this ''transition'' radius is nearly the
same for both of our adopted B-field models. We then solve analytically for the
torques on the central star and for the disk luminosity due to gravity and
magnetic torques. When expressed in a dimensionless form, the resulting
quantities depend on one parameter alone, the ratio of the transition radius to
the corotation radius. For rapid rotators, the accretion disk may be powered
mostly by spin-down of the central star. These results are independent of the
viscosity prescription in the disk. We also solve for the disk structure for
the special case of an optically thick alpha disk. Our results are applicable
to a range of astrophysical systems including accreting neutron stars,
intermediate polar cataclysmic variables, and T Tauri systems.Comment: 9 sharper figs, updated reference
On the rotational dynamics of magnetically threaded disks around neutron stars
We investigate the rotational dynamics of disk accretion around a strongly magnetized neutron star with an aligned dipole field. The magnetospheric field is assumed to thread the disk plasma both inside and outside the corotation radius. As a result of disk-star interaction, the magnetic torque on the disk affects the structure of accretion flow to yield the observed spin- up or spin- down rates for a source of given fastness, magnetic field strength, and mass accretion rate. Within the model we obtain a prescription for the dynamical viscosity of such magnetically modified solutions for a Keplerian disk. We then use this prescription to find a model solution for the rotation rate profile throughout the entire disk, including the non-Keplerian inner disk. We find that the non-Keplerian angular velocity transition region is not necessarily narrow for a source of given spin state. The boundary layer approximation, as in the standard magnetically threaded disk model, holds only in the case of dynamical viscosity decreasing all the way to the innermost edge of the disk. These results are applied to several observed disk-fed X-ray pulsars that have exhibited quasi-periodic oscillations (QPOs). The QPO frequencies provide a constraint on the fastness parameter and enable one to determine uniquely the width of the angular velocity transition zone for each source within model assumptions. We discuss the implications of these results on the value of the critical fastness parameter for a magnetized star in spin equilibrium. Applications of our model are also made with relevant parameters from recent numerical simulations of quasi-stationary disk - magnetized star interactions
Stability of spherical stellar systems II : Numerical results
We have performed a series of high resolution N-body experiments on a
Connection Machine CM-5 in order to study the stability of collisionless
self-gravitating spherical systems. We interpret our results in the framework
of symplectic mechanics, which provides the definition of a new class of
particular perturbations: The preserving perturbations, which are a
generalization of the radial ones. Using models defined by the Ossipkov-Merritt
algorithm, we show that the stability of a spherical anisotropic system is
directly related to the preserving or non-preserving nature of the
perturbations acting on the system. We then generalize our results to all
spherical systems. Since the ``isotropic component'' of the linear variation of
the distribution function cannot be used to predict the stability or
instability of a spherical system, we propose a more useful stability parameter
which is derived from the ``anisotropic'' component of the linear variation.Comment: uuencoded gzip compressed postscript file containing 14 pages,
accepted for publication in MNRA
Warping and Precession of Accretion Disks Around Magnetic Stars: Nonlinear Evolution
The inner region of the accretion disk around a magnetized star (T Tauri
star, white dwarf or neutron star) is subjected to magnetic torques that induce
warping and precession of the disk. These torques arise from the interaction
between the stellar field and the induced electric currents in the disk. We
carry out numerical simulations of the nonlinear evolution of warped, viscous
accretion disks driven by the magnetic torques. We show that the disk can
develop into a highly warped steady state in which the disk attains a fixed
(warped) shape and precesses rigidly. The warp is most pronounced at the disk
inner radius (near the magnetosphere boundary). As the system parameters (such
as accretion rate) change, the disk can switch between a completely flat state
(warping stable) and a highly warped state. The precession of warped disks may
be responsible for a variety of quasi-periodic oscillations or radiation flux
variabilities observed in many different systems, including young stellar
objects and X-ray binaries.Comment: 16 pages, 7 figures; extended parameter searches, changes in
discussion; accepted for publication in Ap
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