46 research outputs found
Constraint on the ejecta mass for a black hole-neutron star merger event candidate S190814bv
We derive the upper limit to the ejecta mass of S190814bv, a black
hole-neutron star merger candidate, through the radiative transfer simulations
for kilonovae with the realistic ejecta density profile as well as the detailed
opacity and heating rate models. The limits to the ejecta mass strongly depend
on the viewing angle. For the face-on observations (), the total
ejecta mass should be smaller than for the average distance of
S190814bv ( Mpc), while larger mass is allowed for the edge-on
observations. We also derive the conservative upper limits of the dynamical
ejecta mass to be , , and for the
viewing angle , , and for ,
respectively. We show that the {\it iz}-band observation deeper than mag
within 2 d after the GW trigger is crucial to detect the kilonova with the
total ejecta mass of at the distance of Mpc. We also
show that a strong constraint on the NS mass-radius relation can be obtained if
the future observations put the upper limit of to the dynamical
ejecta mass for a BH-NS event with the chirp mass smaller than and effective spin larger than .Comment: 16 pages, 15 figure
Extracting the cutoff frequency in the gravitational-wave spectrum of black hole-neutron star mergers
The location of the cutoff in the gravitational-wave spectrum of black
hole-neutron star mergers is correlated strongly with the neutron-star radius
for the case that the neutron star is disrupted by the black hole during the
merger. However, the modulation which appears in the spectrum due to the mode
mixing makes it difficult to measure the cutoff frequency if gravitational
waves are observed from inclined direction or the binary is precessing. In this
letter, we show that the cutoff frequency can be measured even in such
situations with a method we have recently proposed to reconstruct the face-on
waveforms only from the strain observed from a particular direction. We show
that the systematic error in the measurement of the neutron-star radius can be
reduced to for the case that tidal disruption of the neutron
star occurs significantly.Comment: 6 pages, 2 figure
Extracting the orbital axis from gravitational waves of precessing binary systems
We present a new method for extracting the instantaneous orbital axis only
from gravitational wave strains of precessing binary systems observed from a
particular observer direction. This method enables us to reconstruct the
co-precessing frame waveforms only from observed quantities for the ideal case
that the signal-to-noise ratio is high enough to analyze the waveforms
directly. Specifically, we do not assume knowledge of the time evolution of the
instantaneous orbital axis and the co-precessing waveforms before analyzing the
data in our method. We test and measure the accuracy of our method using the
numerical relativity simulation data of precessing binary black holes taken
from the SXS Catalog. We show that the direction of the orbital axis is
extracted within error from gravitational waves emitted
during the inspiral phase. The co-precessing waveforms are also reconstructed
with high accuracy; the mismatch (assuming white noise) between them and the
original co-precessing waveforms is typically a few times including
the merger-ringdown phase, and can be improved by an order of magnitude
focusing only on the inspiral waveform. In this method, the co-precessing frame
waveforms are not only the purely technical tools for understanding the complex
nature of precessing waveforms but also direct observables.Comment: 12 pages, 8 figures, 1 table, published in PR
A Monte-Carlo based relativistic radiation hydrodynamics code with a higher-order scheme
We develop a new relativistic radiation hydrodynamics code based on the
Monte-Carlo algorithm. In this code, we implement a new scheme to achieve the
second-order accuracy in time in the limit of a large packet number for solving
the interaction between matter and radiation. This higher-order time
integration scheme is implemented in the manner to guarantee the
energy-momentum conservation to the precision of the geodesic integrator. The
spatial dependence of radiative processes, such as the packet propagation,
emission, absorption, and scattering, are also taken into account up to the
second-order accuracy. We validate our code by solving various test-problems
following the previous studies; one-zone thermalization, dynamical diffusion,
radiation dragging, radiation mediated shock-tube, shock-tube in the optically
thick limit, and Eddington limit problems. We show that our code reproduces
physically appropriate results with reasonable accuracy and also demonstrate
that the second-order accuracy in time and space is indeed achieved with our
implementation for one-zone and one-dimensional problems.Comment: 25 pages, 10 figures, submitted to PR
Radiative transfer simulation for the optical and near-infrared electromagnetic counterparts to GW170817
Recent detection of gravitational waves from a binary-neutron star merger
(GW170817) and the subsequent observations of electromagnetic counterparts
provide a great opportunity to study the physics of compact binary mergers. The
optical and near-infrared counterparts to GW170817 (SSS17a, also known as AT
2017gfo or DLT17ck) are found to be consistent with a kilonova/macronova
scenario with red and blue components. However, in most of previous studies in
which contribution from each ejecta component to the lightcurves is separately
calculated and composited, the red component is too massive as dynamical ejecta
and the blue component is too fast as post-merger ejecta. In this letter, we
perform a 2-dimensional radiative transfer simulation for a kilonova/macronova
consistently taking the interplay of multiple ejecta components into account.
We show that the lightcurves and photospheric velocity of SSS17a can be
reproduced naturally by a setup consistent with the prediction of the
numerical-relativity simulations.Comment: 6 pages, 3 figure
Frequency-domain gravitational waveform models for inspiraling binary neutron stars
We develop a model for frequency-domain gravitational waveforms from
inspiraling binary neutron stars. Our waveform model is calibrated by
comparison with hybrid waveforms constructed from our latest high-precision
numerical-relativity waveforms and the SEOBNRv2T waveforms in the frequency
range of --. We show that the phase difference between our
waveform model and the hybrid waveforms is always smaller than for the binary tidal deformability, , in the range
and for the mass ratio between 0.73
and 1. We show that, for --, the distinguishability for the
signal-to-noise ratio and the mismatch between our waveform model
and the hybrid waveforms are always smaller than 0.25 and ,
respectively. The systematic error of our waveform model in the measurement of
is always smaller than with respect to the hybrid
waveforms for . The statistical error
in the measurement of binary parameters is computed employing our waveform
model, and we obtain results consistent with the previous studies. We show that
the systematic error of our waveform model is always smaller than
(typically smaller than ) of the statistical error for events with the
signal-to-noise ratio of .Comment: 22 pages, 16 figures, accepted for publication in PR
Towards rapid transient identification and characterization of kilonovae
With the increasing sensitivity of advanced gravitational wave detectors, the
first joint detection of an electromagnetic and gravitational wave signal from
a compact binary merger will hopefully happen within this decade. However,
current gravitational-wave likelihood sky areas span , and thus it is a challenging task to identify which,
if any, transient corresponds to the gravitational-wave event. In this study,
we make a comparison between recent kilonovae/macronovae lightcurve models for
the purpose of assessing potential lightcurve templates for counterpart
identification. We show that recent analytical and parametrized models for
these counterparts result in qualitative agreement with more complicated
radiative transfer simulations. Our analysis suggests that with improved
lightcurve models with smaller uncertainties, it will become possible to
extract information about ejecta properties and binary parameters directly from
the lightcurve measurement. Even tighter constraints are obtained in cases for
which gravitational-wave and kilonovae parameter estimation results are
combined. However, to be prepared for upcoming detections, more realistic
kilonovae models are needed. These will require numerical relativity with more
detailed microphysics, better radiative transfer simulations, and a better
understanding of the underlying nuclear physics
Sub-radian-accuracy gravitational waveforms of coalescing binary neutron stars in numerical relativity
Extending our previous studies, we perform high-resolution simulations of
inspiraling binary neutron stars in numerical relativity. We thoroughly carry
through a convergence study in our currently available computational resources
with the smallest grid spacing of --86~meter for the neutron-star
radius 10.9--13.7\,km. The estimated total error in the gravitational-wave
phase is of order 0.1~rad for the total phase of \,rad in the last
--16 inspiral orbits. We then compare the waveforms (without
resolution extrapolation) with those calculated by the latest
effective-one-body formalism (tidal SEOBv2 model referred to as TEOB model). We
find that for any of our models of binary neutron stars, the waveforms
calculated by the TEOB formalism agree with the numerical-relativity waveforms
up to \,ms before the peak of the gravitational-wave amplitude is
reached: For this late inspiral stage, the total phase error is \,rad. Although the gravitational waveforms have an inspiral-type feature
for the last \,ms, this stage cannot be well reproduced by the current
TEOB formalism, in particular, for neutron stars with large tidal deformability
(i.e., lager radius). The reason for this is described.Comment: 13 pages, 11 figures, submitted to PR