2,123 research outputs found
Improving the NRTidal model for binary neutron star systems
Accurate and fast gravitational waveform (GW) models are essential to extract
information about the properties of compact binary systems that generate GWs.
Building on previous work, we present an extension of the NRTidal model for
binary neutron star (BNS) waveforms. The upgrades are: (i) a new closed-form
expression for the tidal contribution to the GW phase which includes further
analytical knowledge and is calibrated to more accurate numerical relativity
data than previously available; (ii) a tidal correction to the GW amplitude;
(iii) an extension of the spin-sector incorporating equation-of-state-dependent
finite size effects at quadrupolar and octupolar order; these appear in the
spin-spin tail terms and cubic-in-spin terms, both at 3.5PN. We add the new
description to the precessing binary black hole waveform model IMRPhenomPv2 to
obtain a frequency-domain precessing binary neutron star model. In addition, we
extend the SEOBNRv4_ROM and IMRPhenomD aligned-spin binary black hole waveform
models with the improved tidal phase corrections. Focusing on the new
IMRPhenomPv2_NRTidalv2 approximant, we test the model by comparing with
numerical relativity waveforms as well as hybrid waveforms combining tidal
effective-one-body and numerical relativity data. We also check consistency
against a tidal effective-one-body model across large regions of the BNS
parameter space.Comment: Accepted manuscrip
Effect of Ignoring Eccentricity in Testing General Relativity with Gravitational Waves
Detections of gravitational waves emitted from binary black hole coalescences
allow us to probe the strong-field dynamics of general relativity (GR). One can
compare the observed gravitational-wave signals with theoretical waveform
models to constrain possible deviations from GR. Any physics that is not
included in these waveform models might show up as apparent GR deviations. The
waveform models used in current tests of GR describe binaries on quasicircular
orbits, since most of the binaries detected by ground-based gravitational-wave
detectors are expected to have negligible eccentricities. Thus, a signal from
an eccentric binary in GR is likely to show up as a deviation from GR in the
current implementation of these tests. We study the response of four standard
tests of GR to eccentric binary black hole signals with the forecast O4
sensitivity of the LIGO-Virgo network. Specifically, we consider two
parameterized tests (TIGER and FTI), the modified dispersion relation test, and
the inspiral-merger-ringdown consistency test. To model eccentric signals, we
use non-spinning numerical relativity simulations from the SXS catalog with
three mass ratios , which we scale to a redshifted total mass of
and luminosity distance of Mpc. For each of these mass
ratios, we consider signals with eccentricities of and at
Hz. We find that signals with larger eccentricity lead to very significant
false GR deviations in most tests while signals having smaller eccentricity
lead to significant deviations in some tests. For the larger eccentricity
cases, one would even get a deviation from GR with TIGER at
credibility at a distance of Gpc. Thus, it will be necessary to
exclude the possibility of an eccentric binary in order to make any claim about
detecting a deviation from GR.Comment: 16 pages, 6 figures, version accepted by PR
Inferring spin tilts at formation from gravitational wave observations of binary black holes: Interfacing precession-averaged and orbit-averaged spin evolution
Two important parameters inferred from the gravitational wave signals of
binaries of precessing black holes are the spin tilt angles, i.e., the angles
at which the black holes' spin axes are inclined with respect to the binary's
orbital angular momentum. The LIGO-Virgo parameter estimation analyses
currently provide spin tilts at a fiducial reference frequency, often the
lowest frequency used in the data analysis. However, the most astrophysically
interesting quantities are the spin tilts when the binary was formed, which can
be significantly different from those at the reference frequency for strongly
precessing binaries. The spin tilts at formally infinite separation are a good
approximation to the tilts at formation in many formation channels and can be
computed efficiently for binary black holes using precession-averaged
evolution. Here, we present a new code for computing the tilts at infinity that
combines the precession-averaged evolution with orbit-averaged evolution at
high frequencies and illustrate its application to GW190521 and other binary
black hole detections from O3a. We have empirically determined the transition
frequency between the orbit-averaged and precession-averaged evolution to
produce tilts at infinity with a given accuracy. We also have regularized the
precession-averaged equations in order to obtain good accuracy for the very
close-to-equal-mass binary parameters encountered in practice. This
additionally allows us to investigate the singular equal-mass limit of the
precession-averaged expressions, where we find an approximate scaling of with the mass ratio .Comment: 25 pages, 16 figure
Binary Neutron Stars with Generic Spin, Eccentricity, Mass ratio, and Compactness - Quasi-equilibrium Sequences and First Evolutions
Information about the last stages of a binary neutron star inspiral and the
final merger can be extracted from quasi-equilibrium configurations and
dynamical evolutions. In this article, we construct quasi-equilibrium
configurations for different spins, eccentricities, mass ratios, compactnesses,
and equations of state. For this purpose we employ the SGRID code, which allows
us to construct such data in previously inaccessible regions of the parameter
space. In particular, we consider spinning neutron stars in isolation and in
binary systems; we incorporate new methods to produce highly eccentric and
eccentricity reduced data; we present the possibility of computing data for
significantly unequal-mass binaries; and we create equal-mass binaries with
individual compactness up to 0.23. As a proof of principle, we explore the
dynamical evolution of three new configurations. First, we simulate a
mass ratio which is the highest mass ratio for a binary neutron star evolved in
numerical relativity to date. We find that mass transfer from the companion
star sets in a few revolutions before merger and a rest mass of
is transferred between the two stars. This configuration
also ejects a large amount of material during merger, imparting a substantial
kick to the remnant. Second, we simulate the first merger of a precessing
binary neutron star. We present the dominant modes of the gravitational waves
for the precessing simulation, where a clear imprint of the precession is
visible in the (2,1) mode. Finally, we quantify the effect of an eccentricity
reduction procedure on the gravitational waveform. The procedure improves the
waveform quality and should be employed in future precision studies, but also
other errors, notably truncation errors, need to be reduced in order for the
improvement due to eccentricity reduction to be effective. [abridged]Comment: (37pages, 26 figures
Linking Quantitative Motor Assessments to the Underlying Brian Injury: A Preliminary Report
Using custom software and an inexpensive novel motion capture controller, we adapted and automated traditional subjective motor assessments in an integrated system to develop a quantitative motor assessment (QMA) that is low-cost, and highly sensitive. Twelve participants who have suffered a traumatic brain injury performed the QMA and had MRI scans of their brain. We compared the individual QMA results from the TBI group to normative standards (developed in an earlier work). We also compared the QMA results to measures of damage found in MRI results. Preliminary analysis of a subset of data are reported here
Shear modulus of the hadron-quark mixed phase
Robust arguments predict that a hadron-quark mixed phase may exist in the
cores of some "neutron" stars. Such a phase forms a crystalline lattice with a
shear modulus higher than that of the crust due to the high density and charge
separation, even allowing for the effects of charge screening. This may lead to
strong continuous gravitational-wave emission from rapidly rotating neutron
stars and gravitational-wave bursts associated with magnetar flares and pulsar
glitches. We present the first detailed calculation of the shear modulus of the
mixed phase. We describe the quark phase using the bag model plus first-order
quantum chromodynamics corrections and the hadronic phase using relativistic
mean-field models with parameters allowed by the most massive pulsar. Most of
the calculation involves treating the "pasta phases" of the lattice via
dimensional continuation, and we give a general method for computing
dimensionally continued lattice sums including the Debye model of charge
screening. We compute all the shear components of the elastic modulus tensor
and angle average them to obtain the effective (scalar) shear modulus for the
case where the mixed phase is a polycrystal. We include the contributions from
changing the cell size, which are necessary for the stability of the
lower-dimensional portions of the lattice. Stability also requires a minimum
surface tension, generally tens of MeV/fm^2 depending on the equation of state.
We find that the shear modulus can be a few times 10^33 erg/cm^3, two orders of
magnitude higher than the first estimate, over a significant fraction of the
maximum mass stable star for certain parameter choices.Comment: 22 pages, 12 figures, version accepted by Phys. Rev. D, with the
corrections to the shear modulus computation and Table I given in the erratu
White matter integrity and vulnerability to Alzheimer's disease: Preliminary findings and future directions
AbstractNeuroimaging biomarkers that precede cognitive decline have the potential to aid early diagnosis of Alzheimer's disease (AD). A body of diffusion tensor imaging (DTI) work has demonstrated declines in white matter (WM) microstructure in AD and its typical prodromal state, amnestic mild cognitive impairment. The present review summarizes recent evidence suggesting that WM integrity declines are present in individuals at high AD-risk, prior to cognitive decline. The available data suggest that AD-risk is associated with WM integrity declines in a subset of tracts showing decline in symptomatic AD. Specifically, AD-risk has been associated with WM integrity declines in tracts that connect gray matter structures associated with memory function. These tracts include parahippocampal WM, the cingulum, the inferior fronto-occipital fasciculus, and the splenium of the corpus callosum. Preliminary evidence suggests that some AD-risk declines are characterized by increases of radial diffusivity, raising the possibility that a myelin-related pathology may contribute to AD onset. These findings justify future research aimed at a more complete understanding of the neurobiological bases of DTI-based declines in AD. With continued refinement of imaging methods, DTI holds promise as a method to aid identification of presymptomatic AD. This article is part of a Special Issue entitled: Imaging Brain Aging and Neurodegenerative disease
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