2,052 research outputs found
Estimating spinning binary parameters and testing alternative theories of gravity with LISA
We investigate the effect of spin-orbit and spin-spin couplings on the
estimation of parameters for inspiralling compact binaries of massive black
holes, and for neutron stars inspiralling into intermediate-mass black holes,
using hypothetical data from the proposed Laser Interferometer Space Antenna
(LISA). We work both in Einstein's theory and in alternative theories of
gravity of the scalar-tensor and massive-graviton types. We restrict the
analysis to non-precessing spinning binaries, i.e. to cases where the spins are
aligned normal to the orbital plane. We find that the accuracy with which
intrinsic binary parameters such as chirp mass and reduced mass can be
estimated within general relativity is degraded by between one and two orders
of magnitude. We find that the bound on the coupling parameter omega_BD of
scalar-tensor gravity is significantly reduced by the presence of spin
couplings, while the reduction in the graviton-mass bound is milder. Using fast
Monte-Carlo simulations of 10^4 binaries, we show that inclusion of spin terms
in massive black-hole binaries has little effect on the angular resolution or
on distance determination accuracy. For stellar mass inspirals into
intermediate-mass black holes, the angular resolution and the distance are
determined only poorly, in all cases considered. We also show that, if LISA's
low-frequency noise sensitivity can be extrapolated from 10^-4 Hz to as low as
10^-5 Hz, the accuracy of determining both extrinsic parameters (distance, sky
location) and intrinsic parameters (chirp mass, reduced mass) of massive
binaries may be greatly improved.Comment: 29 pages, 9 figures. Matches version accepted in Physical Review D.
More stringent checks in the inversion of the Fisher matri
Final spins from the merger of precessing binary black holes
The inspiral of binary black holes is governed by gravitational radiation
reaction at binary separations r < 1000 M, yet it is too computationally
expensive to begin numerical-relativity simulations with initial separations r
> 10 M. Fortunately, binary evolution between these separations is well
described by post-Newtonian equations of motion. We examine how this
post-Newtonian evolution affects the distribution of spin orientations at
separations r ~ 10 M where numerical-relativity simulations typically begin.
Although isotropic spin distributions at r ~ 1000 M remain isotropic at r ~ 10
M, distributions that are initially partially aligned with the orbital angular
momentum can be significantly distorted during the post-Newtonian inspiral.
Spin precession tends to align (anti-align) the binary black hole spins with
each other if the spin of the more massive black hole is initially partially
aligned (anti-aligned) with the orbital angular momentum, thus increasing
(decreasing) the average final spin. Spin precession is stronger for
comparable-mass binaries, and could produce significant spin alignment before
merger for both supermassive and stellar-mass black hole binaries. We also
point out that precession induces an intrinsic accuracy limitation (< 0.03 in
the dimensionless spin magnitude, < 20 degrees in the direction) in predicting
the final spin resulting from the merger of widely separated binaries.Comment: 20 pages, 16 figures, new PN terms, submitted to PR
Distinguishing double neutron star from neutron star-black hole binary populations with gravitational wave observations
Gravitational waves from the merger of two neutron stars cannot be easily
distinguished from those produced by a comparable-mass mixed binary in which
one of the companions is a black hole. Low-mass black holes are interesting
because they could form in the aftermath of the coalescence of two neutron
stars, from the collapse of massive stars, from matter overdensities in the
primordial Universe, or as the outcome of the interaction between neutron stars
and dark matter. Gravitational waves carry the imprint of the internal
composition of neutron stars via the so-called tidal deformability parameter,
which depends on the stellar equation of state and is equal to zero for black
holes. We present a new data analysis strategy powered by Bayesian inference
and machine learning to identify mixed binaries, hence low-mass black holes,
using the distribution of the tidal deformability parameter inferred from
gravitational-wave observations.Comment: 13 pages, 6 figures - v2: matches the published version in Phys. Rev.
D 102, 02302
Explaining LIGO's observations via isolated binary evolution with natal kicks
We compare binary evolution models with different assumptions about
black-hole natal kicks to the first gravitational-wave observations performed
by the LIGO detectors. Our comparisons attempt to reconcile merger rate,
masses, spins, and spin-orbit misalignments of all current observations with
state-of-the-art formation scenarios of binary black holes formed in isolation.
We estimate that black holes (BHs) should receive natal kicks at birth of the
order of (50) km/s if tidal processes do (not) realign
stellar spins. Our estimate is driven by two simple factors. The natal kick
dispersion is bounded from above because large kicks disrupt too many
binaries (reducing the merger rate below the observed value). Conversely, the
natal kick distribution is bounded from below because modest kicks are needed
to produce a range of spin-orbit misalignments. A distribution of misalignments
increases our models' compatibility with LIGO's observations, if all BHs are
likely to have natal spins. Unlike related work which adopts a concrete BH
natal spin prescription, we explore a range of possible BH natal spin
distributions. Within the context of our models, for all of the choices of
used here and within the context of one simple fiducial parameterized
spin distribution, observations favor low BH natal spin.Comment: 19 pages, 14 figures, as published in PR
Comment on `Hawking radiation from fluctuating black holes'
Takahashi & Soda (2010 Class. Quantum Grav. v27 p175008, arXiv:1005.0286)
have recently considered the effect (at lowest non-trivial order) of dynamical,
quantized gravitational fluctuations on the spectrum of scalar Hawking
radiation from a collapsing Schwarzschild black hole. However, due to an
unfortunate choice of gauge, the dominant (even divergent) contribution to the
coefficient of the spectrum correction that they identify is a pure gauge
artifact. I summarize the logic of their calculation, comment on the
divergences encountered in its course and comment on how they could be
eliminated, and thus the calculation be completed.Comment: 12 pages, 1 fig; feynmp, amsref
Multiband gravitational-wave event rates and stellar physics
Joint gravitational-wave detections of stellar-mass black-hole binaries by
ground- and space-based observatories will provide unprecedented opportunities
for fundamental physics and astronomy. We present a semianalytic method to
estimate multiband event rates by combining selection effects of ground-based
interferometers (like LIGO/Virgo) and space missions (like LISA). We forecast
the expected number of multiband detections first by using information from
current LIGO/Virgo data, and then through population synthesis simulations of
binary stars. We estimate that few to tens of LISA detections can be used to
predict mergers detectable on the ground. Conversely, hundreds of events could
potentially be extracted from the LISA data stream using prior information from
ground detections. In general, the merger signal of binaries observable by LISA
is strong enough to be unambiguously identified by both current and future
ground-based detectors. Therefore third-generation detectors will not increase
the number of multiband detections compared to LIGO/Virgo. We use population
synthesis simulations of isolated binary stars to explore some of the stellar
physics that could be constrained with multiband events, and we show that
specific formation pathways might be overrepresented in multiband events
compared to ground-only detections.Comment: 17 pages, 11 figures. Database and python code available at
https://github.com/dgerosa/spops - Published in PR
Quasinormal modes of Kerr-Newman black holes: coupling of electromagnetic and gravitational perturbations
We compute numerically the quasinormal modes of Kerr-Newman black holes in
the scalar case, for which the perturbation equations are separable. Then we
study different approximations to decouple electromagnetic and gravitational
perturbations of the Kerr-Newman metric, computing the corresponding
quasinormal modes. Our results suggest that the Teukolsky-like equation derived
by Dudley and Finley gives a good approximation to the dynamics of a rotating
charged black hole for Q<M/2. Though insufficient to deal with Kerr-Newman
based models of elementary particles, the Dudley-Finley equation should be
adequate for astrophysical applications.Comment: 13 pages, 3 figures. Minor changes to match version accepted in Phys.
Rev.
Superkicks in ultrarelativistic encounters of spinning black holes
We study ultrarelativistic encounters of two spinning, equal-mass black holes
through simulations in full numerical relativity. Two initial data sequences
are studied in detail: one that leads to scattering and one that leads to a
grazing collision and merger. In all cases, the initial black hole spins lie in
the orbital plane, a configuration that leads to the so-called "superkicks". In
astrophysical, quasicircular inspirals, such kicks can be as large as ~3,000
km/s; here, we find configurations that exceed ~15,000 km/s. We find that the
maximum recoil is to a good approximation proportional to the total amount of
energy radiated in gravitational waves, but largely independent of whether a
merger occurs or not. This shows that the mechanism predominantly responsible
for the superkick is not related to merger dynamics. Rather, a consistent
explanation is that the "bobbing" motion of the orbit causes an asymmetric
beaming of the radiation produced by the in-plane orbital motion of the binary,
and the net asymmetry is balanced by a recoil. We use our results to formulate
some conjectures on the ultimate kick achievable in any black hole encounter.Comment: 10 pages, 6 figures, 2 table
Matched-filtering and parameter estimation of ringdown waveforms
Using recent results from numerical relativity simulations of non-spinning
binary black hole mergers we revisit the problem of detecting ringdown
waveforms and of estimating the source parameters, considering both LISA and
Earth-based interferometers. We find that Advanced LIGO and EGO could detect
intermediate-mass black holes of mass up to about 1000 solar masses out to a
luminosity distance of a few Gpc. For typical multipolar energy distributions,
we show that the single-mode ringdown templates presently used for ringdown
searches in the LIGO data stream can produce a significant event loss (> 10%
for all detectors in a large interval of black hole masses) and very large
parameter estimation errors on the black hole's mass and spin. We estimate that
more than 10^6 templates would be needed for a single-stage multi-mode search.
Therefore, we recommend a "two stage" search to save on computational costs:
single-mode templates can be used for detection, but multi-mode templates or
Prony methods should be used to estimate parameters once a detection has been
made. We update estimates of the critical signal-to-noise ratio required to
test the hypothesis that two or more modes are present in the signal and to
resolve their frequencies, showing that second-generation Earth-based detectors
and LISA have the potential to perform no-hair tests.Comment: 19 pages, 9 figures, matches version in press in PR
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