1,412 research outputs found
3D simulations of gyrosynchrotron emission from mildly anisotropic nonuniform electron distributions in symmetric magnetic loops
Microwave emission of solar flares is formed primarily by incoherent
gyrosynchrotron radiation generated by accelerated electrons in coronal
magnetic loops. The resulting emission depends on many factors, including
pitch-angle distribution of the emitting electrons and the source geometry. In
this work, we perform systematic simulations of solar microwave emission using
recently developed tools (GS Simulator and fast gyrosynchrotron codes) capable
of simulating maps of radio brightness and polarization as well as spatially
resolved emission spectra. A 3D model of a symmetric dipole magnetic loop is
used. We compare the emission from isotropic and anisotropic (of loss-cone
type) electron distributions. We also investigate effects caused by
inhomogeneous distribution of the emitting particles along the loop. It is
found that effect of the adopted moderate electron anisotropy is the most
pronounced near the footpoints and it also depends strongly on the loop
orientation. Concentration of the emitting particles at the loop top results in
a corresponding spatial shift of the radio brightness peak, thus reducing
effects of the anisotropy. The high-frequency (around 50 GHz) emission spectral
index is specified mainly by the energy spectrum of the emitting electrons;
however, at intermediate frequencies (around 10-20 GHz), the spectrum shape is
strongly dependent on the electron anisotropy, spatial distribution, and
magnetic field nonuniformity. The implications of the obtained results for the
diagnostics of the energetic electrons in solar flares are discussed.Comment: ApJ in press. 20 pp, 13 figs, on-line album and simulation source
code availabl
Diffusive synchrotron radiation from extragalactic jets
Flattenings of nonthermal radiation spectra observed from knots and interknot
locations of the jets of 3C273 and M87 in UV and X-ray bands are discussed
within modern models of magnetic field generation in the relativistic jets.
Specifically, we explicitly take into account the effect of the small-scale
random magnetic field, probably present in such jets, which gives rise to
emission of Diffusive Synchrotron Radiation, whose spectrum deviates
substantially from the standard synchrotron spectrum, especially at high
frequencies. The calculated spectra agree well with the observed ones if the
energy densities contained in small-scale and large-scale magnetic fields are
comparable. The implications of this finding for magnetic field generation,
particle acceleration, and jet composition are discussed.Comment: 5 pages with 2 figures, MNRAS Letters, accepte
Radio emission from acceleration sites of solar flares
The Letter takes up a question of what radio emission is produced by
electrons at the very acceleration site of a solar flare. Specifically, we
calculate incoherent radio emission produced within two competing acceleration
models--stochastic acceleration by cascading MHD turbulence and regular
acceleration in collapsing magnetic traps. Our analysis clearly demonstrates
that the radio emission from the acceleration sites: (i) has sufficiently
strong intensity to be observed by currently available radio instruments and
(ii) has spectra and light curves which are distinctly different in these two
competing models, which makes them observationally distinguishable. In
particular, we suggest that some of the narrowband microwave and decimeter
continuum bursts may be a signature of the stochastic acceleration in solar
flares.Comment: ApJL, in pres
GRB spectral parameter modeling
Fireball model of the gamma-ray bursts (GRBs) predicts generation of numerous
internal shocks, which efficiently accelerate charged particles and generate
relatively small-scale stochastic magnetic and electric fields. The accelerated
particles diffuse in space due to interaction with the random waves and so emit
so called Diffusive Synchrotron Radiation (DSR) in contrast to standard
synchrotron radiation they would produce in a large-scale regular magnetic
fields. In this contribution we present key results of detailed modeling of the
GRB spectral parameters, which demonstrate that the non-perturbative DSR
emission mechanism in a strong random magnetic field is consistent with
observed distributions of the Band parameters and also with cross-correlations
between them.Comment: 3 pages; IAU symposium # 274 "Advances in Plasma Astrophysics
Diffusive radiation in Langmuir turbulence produced by jet shocks
Anisotropic distributions of charged particles including two-stream
distributions give rise to generation of either stochastic electric fields (in
the form of Langmuir waves, Buneman instability) or random quasi-static
magnetic fields (Weibel and filamentation instabilities) or both. These
two-stream instabilities are known to play a key role in collisionless shock
formation, shock-shock interactions, and shock-induced electromagnetic
emission. This paper applies the general non-perturbative stochastic theory of
radiation to study electromagnetic emission produced by relativistic particles,
which random walk in the stochastic electric fields of the Langmuir waves. This
analysis takes into account the cumulative effect of uncorrelated Langmuir
waves on the radiating particle trajectory giving rise to angular diffusion of
the particle, which eventually modifies the corresponding radiation spectra. We
demonstrate that the radiative process considered is probably relevant for
emission produced in various kinds of astrophysical jets, in particular, prompt
gamma-ray burst spectra, including X-ray excesses and prompt optical flashes.Comment: 9 pages, 5 figures, MNRAS, accepte
Modeling of gyrosynchrotron radio emission pulsations produced by MHD loop oscillations in solar flares
A quantitative study of the observable radio signatures of the sausage, kink,
and torsional MHD oscillation modes in flaring coronal loops is performed.
Considering first non-zero order effect of these various MHD oscillation modes
on the radio source parameters such as magnetic field, line of sight, plasma
density and temperature, electron distribution function, and the source
dimensions, we compute time dependent radio emission (spectra and light
curves). The radio light curves (of both flux density and degree of
polarization) at all considered radio frequencies are than quantified in both
time domain (via computation of the full modulation amplitude as a function of
frequency) and in Fourier domain (oscillation spectra, phases, and partial
modulation amplitude) to form the signatures specific to a particular
oscillation mode and/or source parameter regime. We found that the parameter
regime and the involved MHD mode can indeed be distinguished using the
quantitative measures derived in the modeling. We apply the developed approach
to analyze radio burst recorded by Owens Valley Solar Array and report possible
detection of the sausage mode oscillation in one (partly occulted) flare and
kink or torsional oscillations in another flare.Comment: ApJ, accepte
Thermal to Nonthermal Energy Partition at the Early Rise Phase of Solar Flares
In some flares the thermal component appears much earlier than the nonthermal
component in X-ray range. Using sensitive microwave observations we revisit
this finding made by Battaglia et al. (2009) based on RHESSI data analysis. We
have found that nonthermal microwave emission produced by accelerated electrons
with energy of at least several hundred keV, appears as early as the thermal
soft X-ray emission indicative that the electron acceleration takes place at
the very early flare phase. The non-detection of the hard X-rays at that early
stage of the flares is, thus, an artifact of a limited RHESSI sensitivity. In
all considered events, the microwave emission intensity increases at the early
flare phase. We found that either thermal or nonthermal gyrosynchrotron
emission can dominate the low-frequency part of the microwave spectrum below
the spectral peak occurring at 3-10 GHz. In contrast, the high-frequency
optically thin part of the spectrum is always formed by the nonthermal,
accelerated electron component, whose power-law energy spectrum can extend up
to a few MeV at this early flare stage. This means that even though the total
number of accelerated electrons is small at this stage, their nonthermal
spectrum is fully developed. This implies that an acceleration process of
available seed particles is fully operational. While, creation of this seed
population (the process commonly called `injection' of the particles from the
thermal pool into acceleration) has a rather low efficiency at this stage,
although, the plasma heating efficiency is high. This imbalance between the
heating and acceleration (in favor of the heating) is difficult to reconcile
within most of available flare energization models. Being reminiscent of the
tradeoff between the Joule heating and runaway electron acceleration, it puts
additional constraints on the electron injection into the acceleration process.Comment: 11 pages, 12 figures, accepted for Ap
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