15,483 research outputs found
Relativistic Neutron Stars: Rheological Type Extensions of the Equations of State
Based on the Rheological Paradigm, one has extended the equations of state
for relativistic spherically symmetric static neutron stars, taking into
consideration the derivative of the matter pressure along the so-called
director four-vector. The modified equations of state are applied to the model
of a zero-temperature neutron condensate. This model includes one new parameter
with the dimensionality of length, which describes the rheological type
screening inside the neutron star. As an illustration of the new approach, one
has considered the rheological type generalization of the non-relativistic
Lane-Emden theory and found the numerical profiles of the pressure for a number
of values of the new guiding parameter. One has found that the rheological type
self-interaction makes the neutron star more compact, since the radius of the
star, related to the first null of the pressure profile, decreases when the
modulus of the rheological type guiding parameter grows.Comment: 14 pages, 1 figure, 1 tabl
Anisotropic stars as ultracompact objects in General Relativity
Anisotropic stresses are ubiquitous in nature, but their modeling in General
Relativity is poorly understood and frame dependent. We introduce the first
study on the dynamical properties of anisotropic self-gravitating fluids in a
covariant framework. Our description is particularly useful in the context of
tests of the black hole paradigm, wherein ultracompact objects are used as
black hole mimickers but otherwise lack a proper theoretical framework. We show
that: (i) anisotropic stars can be as compact and as massive as black holes,
even for very small anisotropy parameters; (ii) the nonlinear dynamics of the
1+1 system is in good agreement with linearized calculations, and shows that
configurations below the maximum mass are nonlinearly stable; (iii) strongly
anisotropic stars have vanishing tidal Love numbers in the black-hole limit;
(iv) their formation will usually be accompanied by gravitational-wave echoes
at late times.Comment: 7+2 pages, 6 figures; v2: include extra material (general covariant
framework for anisotropic fluids in General Relativity without symmetries and
code validation); to appear in PR
Maximum mass and universal relations of rotating relativistic hybrid hadron-quark stars
We construct equilibrium models of uniformly and differentially rotating
hybrid hadron-quark stars using equations of state (EOSs) with a first-order
phase transition that gives rise to a third family of compact objects. We find
that the ratio of the maximum possible mass of uniformly rotating
configurations - the supramassive limit - to the Tolman-Oppenheimer-Volkoff
(TOV) limit mass is not EOS-independent, and is between 1.15 and 1.31,in
contrast with the value of 1.20 previously found for hadronic EOSs. Therefore,
some of the constraints placed on the EOS from the observation of the
gravitational wave event GW170817 do not apply to hadron-quark EOSs. However,
the supramassive limit mass for the family of EOSs we treat is consistent with
limits set by GW170817, strengthening the possibility of interpreting GW170817
with a hybrid hadron-quark EOSs. We also find that along constant angular
momentum sequences of uniformly rotating stars, the third family maximum and
minimum mass models satisfy approximate EOS-independent relations, and the
supramassive limit of the third family is approximately 16.5 % larger than the
third family TOV limit. For differentially rotating spheroidal stars, we find
that a lower-limit on the maximum supportable rest mass is 123 % more than the
TOV limit rest mass. Finally, we verify that the recently discovered universal
relations relating angular momentum, rest mass and gravitational mass for
turning-point models hold for hybrid hadron-quark EOSs when uniform rotation is
considered, but have a clear dependence on the degree of differential rotation.Comment: 19 pages, 14 figures, submitted to EPJA Topical Issue "First joint
gravitational wave and electromagnetic observations: Implications for nuclear
and particle physics
Localization theorems for nonlinear eigenvalue problems
Let T : \Omega \rightarrow \bbC^{n \times n} be a matrix-valued function
that is analytic on some simply-connected domain \Omega \subset \bbC. A point
is an eigenvalue if the matrix is singular.
In this paper, we describe new localization results for nonlinear eigenvalue
problems that generalize Gershgorin's theorem, pseudospectral inclusion
theorems, and the Bauer-Fike theorem. We use our results to analyze three
nonlinear eigenvalue problems: an example from delay differential equations, a
problem due to Hadeler, and a quantum resonance computation.Comment: Submitted to SIMAX. 22 pages, 11 figure
Differentially-rotating neutron star models with a parametrized rotation profile
We analyze the impact of the choice rotation law on equilibrium sequences of
relativistic differentially-rotating neutron stars in axisymmetry. The maximum
allowed mass for each model is strongly affected by the distribution of angular
velocity along the radial direction and by the consequent degree of
differential rotation. In order to study the wide parameter space implied by
the choice of rotation law, we introduce a functional form that generalizes the
so called "j-const. law" adopted in all previous work. Using this new rotation
law we reproduce the angular velocity profile of differentially-rotating
remnants from the coalescence of binary neutron stars in various 3-dimensional
dynamical simulations. We compute equilibrium sequences of differentially
rotating stars with a polytropic equation of state starting from the
spherically symmetric static case. By analyzing the sequences at constant
ratio, T/|W|, of rotational kinetic energy to gravitational binding energy, we
find that the parameters that best describe the binary neutron star remnants
cannot produce equilibrium configurations with values of T/|W| that exceed
0.14, the criterion for the onset of the secular instability.Comment: Submitted to A&A, 6 pages, 3 figure
The ESPRI project: astrometric exoplanet search with PRIMA I. Instrument description and performance of first light observations
The ESPRI project relies on the astrometric capabilities offered by the PRIMA
facility of the Very Large Telescope Interferometer for the discovery and study
of planetary systems. Our survey consists of obtaining high-precision
astrometry for a large sample of stars over several years and to detect their
barycentric motions due to orbiting planets. We present the operation
principle, the instrument's implementation, and the results of a first series
of test observations. A comprehensive overview of the instrument infrastructure
is given and the observation strategy for dual-field relative astrometry is
presented. The differential delay lines, a key component of the PRIMA facility
which was delivered by the ESPRI consortium, are described and their
performance within the facility is discussed. Observations of bright visual
binaries are used to test the observation procedures and to establish the
instrument's astrometric precision and accuracy. The data reduction strategy
for astrometry and the necessary corrections to the raw data are presented.
Adaptive optics observations with NACO are used as an independent verification
of PRIMA astrometric observations. The PRIMA facility was used to carry out
tests of astrometric observations. The astrometric performance in terms of
precision is limited by the atmospheric turbulence at a level close to the
theoretical expectations and a precision of 30 micro-arcseconds was achieved.
In contrast, the astrometric accuracy is insufficient for the goals of the
ESPRI project and is currently limited by systematic errors that originate in
the part of the interferometer beamtrain which is not monitored by the internal
metrology system. Our observations led to the definition of corrective actions
required to make the facility ready for carrying out the ESPRI search for
extrasolar planets.Comment: 32 pages, 39 figures, Accepted for publication in Astronomy and
Astrophysic
Nonlinear Analysis of Irregular Variables
The Fourier spectral techniques that are common in Astronomy for analyzing
periodic or multi-periodic light-curves lose their usefulness when they are
applied to unsteady light-curves. We review some of the novel techniques that
have been developed for analyzing irregular stellar light or radial velocity
variations, and we describe what useful physical and astronomical information
can be gained from their use.Comment: 31 pages, to appear as a chapter in `Nonlinear Stellar Pulsation' in
the Astrophysics and Space Science Library (ASSL), Editors: M. Takeuti & D.
Sasselo
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