532 research outputs found
Very High Lorentz Factor Fireballs and Gamma-Ray Burst Spectra
Collisionless entrainment of the surrounding matter imports the relativistic
baryon component in the Gamma-Ray Burst (GRB) fireball frame. We show that half
the fireball energy can be transferred from radiation to the comoving hot
motions of baryons under the photosphere. The yet baryon-poor fireball can
reexpand to a very high Lorentz factor (VHLF) \Gamma ~ 10^3-10^6 by its own
relativistic collisionless pressure beyond the photosphere (so-called
collisionless bulk acceleration), leading to internal and external shocks. A
simple synchrotron emission from the VHLF internal shocks produces (i) the
extra power-law spectral component with variability observed in the Fermi GeV
bursts, up to the TeV range for the future Cherenkov Telescope Array (CTA),
(ii) the GeV onset delay with a weak luminosity dependence t_{delay} ~
L^{-1/5}, and (iii) the spectral break of GRB 090926 by the synchrotron cooling
break or the maximum synchrotron cutoff limited by the dynamical time, not by
the e+- creation cutoff. The relativistic baryon component could also heat the
photospheric thermal photons into the main GRB Band spectrum via pp, p\gamma
(Bethe-Heitler and photomeson), and Coulomb thermalization processes. In this
hot photosphere-internal-external shock model, we can predict the
anticorrelation of ~TeV neutrinos and GeV gamma-rays, which may be detectable
using IceCube. The spectral peak and luminosity (Yonetoku) relation is also
reproduced if the progenitor stars are nearly identical. We also discuss the
steep/shallow decay of early X-ray afterglows and short GRBs.Comment: 21 pages, 6 figures, final version to be published in Progress of
Theoretical Physic
Second and higher-order quasi-normal modes in binary black hole mergers
Black hole (BH) oscillations known as quasi-normal modes (QNMs) are one of
the most important gravitational wave (GW) sources. We propose that higher
perturbative order of QNMs, generated by nonlinear gravitational interaction
near the BHs, are detectable and worth searching for in observations and
simulations of binary BH mergers. We calculate the metric perturbations to
second-order and explicitly regularize the master equation at the horizon and
spatial infinity. We find that the second-order QNMs have frequencies twice the
first-order ones and the GW amplitude is up to ~10% that of the first-order
one. The QNM frequency would also shift blueward up to ~1%. This provides a new
test of general relativity as well as a possible distance indicator.Comment: 5 pages, 1 figure, accepted for publication in PRD Rapid
Communication
Efficiency Crisis of Swift Gamma-Ray Bursts with Shallow X-ray Afterglows: Prior Activity or Time-Dependent Microphysics?
Most X-ray afterglows of gamma-ray bursts (GRBs) observed by the Swift
satellite have a shallow decay phase t^{-1/2} in the first few hours. This is
not predicted by the standard afterglow model and needs an explanation. We
discuss that the shallow decay requires an unreasonably high gamma-ray
efficiency, >75-90%, within current models, which is difficult to produce by
internal shocks. Such a crisis may be avoided if a weak relativistic explosion
occurs ~10^3-10^6 s prior to the main burst or if the microphysical parameter
of the electron energy increases during the shallow decay, \epsilon_e ~
t^{1/2}. The former explanation predicts a very long precursor, while both
prefer dim optical flashes from the reverse shock, as was recently reported. We
also calculate the multi-wavelength afterglows and compare them with
observations. No optical break at the end of the shallow X-ray decay indicates
a preference for the time-dependent microphysics model with additionally
decaying magnetic fields, \epsilon_B ~ t^{-0.6}.Comment: 7 pages, 1 figure, accepted for publication in A&
Second Order Quasi-Normal Mode of the Schwarzschild Black Hole
We formulate and calculate the second order quasi-normal modes (QNMs) of a
Schwarzschild black hole (BH). Gravitational wave (GW) from a distorted BH, so
called ringdown, is well understood as QNMs in general relativity. Since QNMs
from binary BH mergers will be detected with high signal-to-noise ratio by GW
detectors, it is also possible to detect the second perturbative order of QNMs,
generated by nonlinear gravitational interaction near the BH. In the BH
perturbation approach, we derive the master Zerilli equation for the metric
perturbation to second order and explicitly regularize it at the horizon and
spatial infinity. We numerically solve the second order Zerilli equation by
implementing the modified Leaver's continued fraction method. The second order
QNM frequencies are found to be twice the first order ones, and the GW
amplitude is up to that of the first order for the binary BH
mergers. Since the second order QNMs always exist, we can use their detections
(i) to test the nonlinearity of general relativity, in particular the no-hair
theorem, (ii) to remove fake events in the data analysis of QNM GWs and (iii)
to measure the distance to the BH.Comment: 23 pages, no figur
Gravitational Wave Memory of Gamma-Ray Burst Jets
Gamma-Ray Bursts (GRBs) are now considered as relativistic jets. We analyze
the gravitational waves from the acceleration stage of the GRB jets. We show
that (i) the point mass approximation is not appropriate if the opening
half-angle of the jet is larger than the inverse of the Lorentz factor of the
jet, (ii) the gravitational waveform has many step function like jumps, and
(iii) the practical DECIGO and BBO may detect such an event if the GRBs occur
in Local group of galaxy. We found that the light curve of GRBs and the
gravitational waveform are anti-correlated so that the detection of the
gravitational wave is indispensable to determine the structure of GRB jets.Comment: Revtex4, 10 pages, 6 figures, Fig.2 and Fig.3 replaced, minor changes
to text in Sec.I and Sec.V, typos corrected, some reference added, Version to
be published in PR
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