132 research outputs found
Neutron star tidal deformability and equation of state constraints
Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars' macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational wave emission, this deformation, quantified through a parameter termed the \emph{tidal deformability}, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature's most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron star coalescence with gravitational waves as of the time of writing
Neutron star tidal deformability and equation of state constraints
Despite their long history and astrophysical importance, some of the key
properties of neutron stars are still uncertain. The extreme conditions
encountered in their interiors, involving matter of uncertain composition at
extreme density and isospin asymmetry, uniquely determine the stars'
macroscopic properties within General Relativity. Astrophysical constraints on
those macroscopic properties, such as neutron star masses and radii, have long
been used to understand the microscopic properties of the matter that forms
them. In this article we discuss another astrophysically observable macroscopic
property of neutron stars that can be used to study their interiors: their
tidal deformation. Neutron stars, much like any other extended object with
structure, are tidally deformed when under the influence of an external tidal
field. In the context of coalescences of neutron stars observed through their
gravitational wave emission, this deformation, quantified through a parameter
termed the \emph{tidal deformability}, can be measured. We discuss the role of
the tidal deformability in observations of coalescing neutron stars with
gravitational waves and how it can be used to probe the internal structure of
Nature's most compact matter objects. Perhaps inevitably, a large portion of
the discussion will be dictated by GW170817, the most informative confirmed
detection of a binary neutron star coalescence with gravitational waves as of
the time of writing.Comment: invited review for General Relativity and Gravitation, published
versio
Toward Realistic and Practical No-Hair Relations for Neutron Stars in the Non-Relativistic Limit
The gravitational properties of astrophysical objects depend sensitively on
their internal structure. In Newtonian theory, the gravitational potential of a
rotating star can be fully described by an infinite number of multipole moments
of its mass distribution. Recently, this infinite number of moments for
uniformly-rotating stars were shown semi-analytically to be expressible in
terms of just the first three: the mass, the spin, and the quadrupole moment of
the star. The relations between the various lower multipole moments were
additionally shown to depend weakly on the equation of state, when considering
neutron stars and assuming single polytropic equations of state. Here we extend
this result in two ways. First, we show that the universality also holds for
realistic equations of state, thus relaxing the need to use single polytropes.
Second, we derive purely analytical universal relations by perturbing the
equations of structure about an polytrope that reproduce semi-analytic
results to . We also find that the linear-order perturbation
vanishes in some cases, which provides further evidence and a deeper
understanding of the universality.Comment: 10 pages, 5 figures, published versio
Tidal heating and torquing of a Kerr black hole to next-to-leading order in the tidal coupling
We calculate the linear vacuum perturbations of a Kerr black hole surrounded
by a slowly-varying external spacetime to third order in the ratio of the
black-hole mass to the radius of curvature of the external spacetime. This
expansion applies to two relevant physical scenarios: (i) a small Kerr black
hole immersed in the gravitational field of a much larger external black hole,
and (ii) a Kerr black hole moving slowly around another external black hole of
comparable mass. This small-hole/slow-motion approximation allows us to
parametrize the perturbation through slowly-varying, time-dependent electric
and magnetic tidal tensors, which then enables us to separate the Teukolsky
equation and compute the Newman-Penrose scalar analytically to third order in
our expansion parameter. We obtain generic expressions for the mass and angular
momentum flux through the perturbed black hole horizon, as well as the rate of
change of the horizon surface area, in terms of certain invariants constructed
from the electric and magnetic tidal tensors. We conclude by applying these
results to the two scenarios described above.Comment: 15 pages, no figures, published versio
On combining information from multiple gravitational wave sources
In the coming years, advanced gravitational wave detectors will observe
signals from a large number of compact binary coalescences. The majority of
these signals will be relatively weak, making the precision measurement of
subtle effects, such as deviations from general relativity, challenging in the
individual events. However, many weak observations can be combined into precise
inferences, if information from the individual signals is combined in an
appropriate way. In this study we revisit common methods for combining multiple
gravitational wave observations to test general relativity, namely (i)
multiplying the individual likelihoods of beyond-general-relativity parameters
and (ii) multiplying the Bayes Factor in favor of general relativity from each
event. We discuss both methods and show that they make stringent assumptions
about the modified theory of gravity they test. In particular, the former
assumes that all events share the same beyond-general-relativity parameter,
while the latter assumes that the theory of gravity has a new unrelated
parameter for each detection. We show that each method can fail to detect
deviations from general relativity when the modified theory being tested
violates these assumptions. We argue that these two methods are the extreme
limits of a more generic framework of hierarchical inference on hyperparameters
that characterize the underlying distribution of single-event parameters. We
illustrate our conclusions first using a simple model of Gaussian likelihoods,
and also by applying parameter estimation techniques to a simulated dataset of
gravitational waveforms in a model where the graviton is massive. We argue that
combining information from multiple sources requires explicit assumptions that
make the results inherently model-dependent.Comment: 9 pages, 3 figure
Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects
The properties of compact binaries, such as masses and spins, are imprinted
in the gravitational-waves they emit and can be measured using parameterised
waveform models. Accurately and efficiently describing the complicated
precessional dynamics of the various angular momenta of the system in these
waveform models is the object of active investigation. One of the key models
extensively used in the analysis of LIGO and Virgo data is the
single-precessing-spin waveform model IMRPhenomPv2. In this article we present
a new model IMRPhenomPv3 which includes the effects of two independent spins in
the precession dynamics. Whereas IMRPhenomPv2 utilizes a single-spin
frequency-dependent post-Newtonian rotation to describe precession effects, the
improved model, IMRPhenomPv3, employs a double-spin rotation that is based on
recent developments in the description of precessional dynamics. Besides
double-spin precession, the improved model benefits from a more accurate
description of precessional effects. We validate our new model against a large
set of precessing numerical-relativity simulations. We find that IMRPhenomPv3
has better agreement with the inspiral portion of precessing binary-black-hole
simulations and is more robust across a larger region of the parameter space
than IMRPhenomPv2. As a first application we analyse, for the first time, the
gravitational-wave event GW151226 with a waveform model that describes two-spin
precession. Within statistical uncertainty our results are consistent with
published results. IMRPhenomPv3 will allow studies of the measurability of
individual spins of binary black holes using GWs and can be used as a
foundation upon which to build further improvements, such as modeling
precession through merger, extending to higher multipoles, and including tidal
effects.Comment: 15 pages, 5 figure
Gravitational Waveforms for Precessing, Quasicircular Compact Binaries with Multiple Scale Analysis: Small Spin Expansion
We obtain analytical gravitational waveforms in the frequency-domain for
precessing, quasi-circular compact binaries with small spins, applicable, for
example, to binary neutron star inspirals. We begin by calculating an analytic
solution to the precession equations, obtained by expanding in the
dimensionless spin parameters and using multiple-scale analysis to separate
timescales. We proceed by analytically computing the Fourier transform of
time-domain waveform through the stationary phase approximation. We show that
the latter is valid for systems with small spins. Finally, we show that these
waveforms have a high overlap with numerical waveforms obtained through direct
integration of the precession equations and discrete Fourier transformations.
The resulting, analytic waveform family is ideal for detection and parameter
estimation of gravitational waves emitted by inspiraling binary neutron stars
with ground-based detectors.Comment: 37 pages, 14 figures, final published versio
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