207 research outputs found
The local energy production rates of GRB photons and of UHECRs
In a recent analysis it was found that the local (z=0) rate at which
gamma-ray bursts (GRBs) produce energy in 1 MeV photons, Q_GRB(z=0), is 300
times lower than the local energy production rate in ultra-high energy
cosmic-rays. This may appear to be in contradiction with earlier results,
according to which Q_GRB(z=0) is similar to the local energy production rate in
>10^{19} eV cosmic-rays, Q_{10EeV}(z=0). This short (1 page) note identifies
the origin of the apparent discrepancy and shows that Q_GRB(z=0) \sim
Q_{10EeV}(z=0) holds.Comment: 1 pag
High energy particles from gamma-ray bursts
A review is presented of the fireball model of gamma-ray bursts (GRBs), and
of the production in GRB fireballs of high energy protons and neutrinos.
Constraints imposed on the model by recent afterglow observations, which
support the association of GRB and ultra-high energy cosmic-ray (UHECR)
sources, are discussed. Predictions of the GRB model for UHECR production,
which can be tested with planned large area UHECR detectors and with planned
high energy neutrino telescopes, are reviewed.Comment: 33 pages. Based on lectures given at the ICTP Summer School (ICTP,
Italy, June 2000), and at the VI Gleb Wataghin School (UNICAMP, Brazil, July
2000
On the origin of fast radio bursts (FRBs)
We derive stringent constraints on the persistent source associated with FRB
121102: Size cm cm, age yr, characteristic
electron energy GeV, total energy erg. The
hot radiating plasma is confined by a cold plasma of mass . The source is nearly resolved, and may be
resolved by 10 GHz observations. The fact that
suggests that the hot plasma was created by the ejection of a mildly
relativistic, shell, which propagated into an extended
ambient medium or collided with a pre-ejected shell of mass . The inferred
plasma properties are inconsistent with typical "magnetar wind nebulae" model
predictions.
We suggest a physical mechanism for the generation of FRBs (independent of
the persistent source model): Ejection from an underlying compact object,
cm, of highly relativistic shells, with energy
erg and Lorentz factor ~, into a surrounding e-p plasma with
density (consistent with that inferred for the plasma producing
the persistent emission associated with FRB 121102). Such shell ejections with
energy typical for FRB events lead to plasma conditions appropriate for strong
synchrotron maser emission at the GHz range, GHz. In this model, a significant fraction of
the deposited energy is converted to an FRB with duration , accompanied
by ~10 MeV photons carrying less energy than the FRB.
The inferred energy and mass associated with the source are low compared to
those of typical supernova ejecta. This may suggest some type of a "weak
stellar explosion", where a neutron star is formed with relatively low mass and
energy ejection. However, the current upper limit on R does not allow one to
rule out .Comment: Accepted to ApJ. 7 pages, 1 figure. Some explanations expanded.
Discussion of beaming added. Some references update
The high energy tail of gamma-ray burst 941017: Comptonization of synchrotron self absorbed photons
The recent detection of an unusually hard spectral component in GRB941017
extending to MeV is hard to explain as a synchrotron emission from
shock-accelerated electrons.
It was argued to imply acceleration of protons to ultra-high energy. We show
here that the "high energy tail" can be explained as emission from
shock-accelerated electrons in the early afterglow epoch, taking into account
the effect of synchrotron self-absorption. High energy observations set in this
case stringent constraints on model parameters: A lower limit to the total
explosion energy E\gsim5 \times 10^{53} erg (assuming spherical symmetry);
An upper limit to the density of gas surrounding the explosion,
n\lsim10^{-2}(E/10^{54}{\rm erg}){\rm cm}^{-3}; A lower limit to the
expansion Lorentz factor \Gamma_i\gsim 200; and An upper limit to the
fraction of thermal energy carried by the magnetic field behind the shock
driven into the surrounding medium,
. Such constraints can not be inferred from
keV--MeV data alone. The unusually low value of and the
unusually high ratio may account for the rareness of GRB941017-type high
energy tails. Tighter constraints on model parameters may be obtained in the
future from optical and sub-TeV observations.Comment: Revised version: Minor changes, 2 graphs combined into 1. Accepted to
ApJ
Properties of the Radio-Emitting Gas Around SgrA*
We show that the radial profiles of the temperature and density of the
electrons as well as the magnetic field strength around the massive black hole
at the Galactic center, SgrA*, may be constrained directly from existing radio
data without any need to make prior assumptions about the dynamics of the
emitting gas. The observed spectrum and wavelength-dependent angular size of
SgrA* indicate that the synchrotron emission originates from an optically-thick
plasma of quasi-thermal electrons. We find that the electron temperature rises
above the virial temperature within tens of Schwarzschild radii from the black
hole, suggesting that the emitting plasma may be outflowing. Constraints on the
electron density profile are derived from polarization measurements. Our
best-fit results differ from expectations based on existing theoretical models.
However, these models cannot be ruled out as of yet due to uncertainties in the
source size measurements. Our constraints could tighten considerably with
future improvements in the size determination and simultaneous polarization
measurements at multiple wavelengths.Comment: 6 pages, 1 figure, accepted for publication in JCAP (Journal of
Cosmology & Astroparticle Physics
Hard X-ray emission from accretion shocks around galaxy clusters
We show that the hard X-ray (HXR) emission observed from several galaxy
clusters is naturally explained by a simple model, in which the nonthermal
emission is produced by inverse Compton scattering of cosmic microwave
background photons by electrons accelerated in cluster accretion shocks: The
dependence of HXR surface brightness on cluster temperature is consistent with
that predicted by the model, and the observed HXR luminosity is consistent with
the fraction of shock thermal energy deposited in relativistic electrons being
\lesssim 0.1. Alternative models, where the HXR emission is predicted to be
correlated with the cluster thermal emission, are disfavored by the data. The
implications of our predictions to future HXR observations (e.g. by NuStar,
Simbol-X) and to (space/ground based) gamma-ray observations (e.g. by Fermi,
HESS, MAGIC, VERITAS) are discussed.Comment: 7 pages, 3 figures, somewhat revised, published in JCA
Nonthermal emission from clusters of galaxies
We show that the spectral and radial distribution of the nonthermal emission
of massive, M>10^{14.5}M_sun, galaxy clusters (GCs) may be approximately
described by simple analytic expressions, which depend on the GC thermal X-ray
properties and on two model parameter, beta_{core} and eta_e. beta_{core} is
the ratio of CR energy density (within a logarithmic CR energy interval) and
the thermal energy density at the GC core, and eta_{e(p)} is the fraction of
the thermal energy generated in strong collisionless shocks, which is deposited
in CR electrons (protons). Using a simple analytic model for the evolution of
ICM CRs, which are produced by accretion shocks (primary CRs), we find that
beta_{core} ~ eta_{p}/200, nearly independent of GC mass and with a scatter
Delta ln(beta_{core}) ~ 1 between GCs of given mass. We show that the HXR and
gamma-ray luminosities produced by IC scattering of CMB photons by primary
electrons exceed the luminosities produced by secondary particles (generated in
hadronic interactions within the GC) by factors ~500(eta_e/eta_p)(T/10
keV)^{-1/2} and ~150(eta_e/eta_p)(T/10 keV)^{-1/2} respectively, where T is the
GC temperature. Secondary particle emission may dominate at the radio and VHE
(> 1 TeV) gamma-ray bands. Our model predicts, in contrast with some earlier
work, that the HXR and gamma-ray emission from GCs are extended, since the
emission is dominated at these energies by primary electrons. Our predictions
are consistent with the observed nonthermal emission of the Coma cluster for
eta_peta_e ~ 0.1. The implications of our predictions to future HXR
observations (e.g. by NuStar, Simbol-X) and to (space/ground based) gamma-ray
observations (e.g. by Fermi, HESS, MAGIC, VERITAS) are discussed. Finally, we
show that our model's results agree with results of detailed numerical
calculations.Comment: 22 pages, 16 figures, somewhat revised, published in JCA
Maser and other instabilities in a weakly magnetized relativistic plasma: Theory and the astrophysical relevance of the maser
A sufficient condition for maser instability in a weakly magnetized
relativistic plasma with an isotropic particle distribution function is given.
The maser growth rates and polarizations are computed starting from the exact
dielectric permittivity tensor of a magnetized plasma. For very weak magnetic
fields, our results confirm the approximate validity of the 'standard maser
theory', which is based on the Einstein coefficients method, with one
significant exception. For inclined propagation and realistic (small but
finite) field, the growth rates of the two (nearly circular) polarizations
differ significantly, while the standard theory predicts two (nearly circular)
polarizations with similar growth rates. We show that this deviation is due to
circularly polarized synchrotron emission, which is neglected in the standard
theory.
The maser is shown to grow slower than Langmuir waves. Nevertheless,
significant generation of EM waves is seen in (highly simplified) direct
numerical simulations. We study the nonlinear saturation of the maser
instability and find that it offers a mechanism for the conversion of a
significant fraction of the plasma energy into radio waves. We briefly discuss
the conditions under which the maser instability may operate in astrophysical
sources, and provide rough estimates that may be used as a guidance when
studying particular astrophysical sources/phenomena
The Cumulative Bakground of High-Energy Neutrinos from Starburst Galaxies
We show that starburst galaxies convert efficiently cosmic-rays into pions,
which in turn decay into high-energy neutrinos and photons. The cumulative
background of GeV neutrinos is 10^{-7}GeV/cm^2/s/sr. Its extrapolation to
higher neutrino energies depends on the energy spectrum of the injected
cosmic-rays and is proportional to E^{-0.15+-0.1} up to E~0.3PeV and possibly
higher neutrino energies. This flux, which constitutes a lower limit to the
high energy extra-Galactic neutrino flux, is likely to be detectable by
forthcoming km-scale neutrino telescopes.Comment: Accepted for publication in JCA
Flavoring Astrophysical Neutrinos: Flavor Ratios Depend on Energy
Electromagnetic (and adiabatic) energy losses of pions and muons modify the
flavor ratio (measured at Earth) of neutrinos produced by pion decay in
astrophysical sources, , from
1:1:1 at low energy to 1:1.8:1.8 at high energy. The transition occurs over 1-2
decades of nuetrino energy, and is correlated with a modification of the
neutrino spectrum. For gamma-ray bursts, e.g., the transition is expected at
\~100 TeV, and may be detected by km-scale neutrino telescopes. Measurements of
the transition energy and energy-width will provide unique probes of the
physics of the sources. pion and muon energy losses also affect the ratio of
flux to total neutrino flux, which may be measured at the
W-resonance (6.3 PeV): It is modified from 1/6 (1/15) at low energy to 1/9
(practically 0) at high energy for neutrinos produced in pp ()
interactions.Comment: v1: 4 pages, 1 figure; v2: added reference; v3: improved
introduction, accepted to PRL; v4: added note about matter oscillation
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