664 research outputs found
The Hard X-rays and Gamma-rays from Solar Flares
Radiation of energies from 10 KeV to greater than 10 MeV has been observed during solar flares, and is interpreted to be due to bremsstrahlung by relativistic electrons. A complete treatment of this problem requires solution of the kinetic equation for relativistic electrons and inclusion of synchrotron energy losses. Using the electron distributions obtained from numerical solutions of this equation the bremsstrahlung spectra in the impulsive x ray and gamma-ray regimes are calculated, and the variation of these spectral indices and directivities with energy and observation angle are described. The dependences of these characteristics of the radiation of changes in the solar atmospheric model, including the convergence of the magnetic field, the injected electron spectral index, and most importantly, in the anisotropy of the injected electrons and of the convergence of the magnetic field are also described. The model results are compared with stereoscopic observations of individual flares and the constraints that this data sets on the models are discussed
Emission, absorption and polarization of gyrosynchrotron radiation of mildly relativistic paricles
Approximate analytic expressions for the emissivity and absorption coefficient of synchrotron radiation of mildly relativistic particles with an arbitrary energy spectrum and pitch angle distribution are given. From these, an expression for the degree of polarization is derived. To accomplish this, previously developed methods of integration are used. The analytic results are compared with numerical results for both thermal and non-thermal (power law) distributions of particles
Looptop Hard X-Ray Emission in Solar Flares: Images and Statistics
The discovery of hard X-ray sources near the top of a flaring loop by the HXT
instrument on board the YOHKOH satellite represents a significant progress
towards the understanding of the basic processes driving solar flares. In this
paper we extend the previous study of limb flares by Masuda (1994) by including
all YOHKOH observations up through August 1998. We report that from October
1991 to August 1998, YOHKOH observed 20 X-ray bright limb flares (where we use
the same selection criteria as Masuda), of which we have sufficient data to
analyze 18 events, including 8 previously unanalyzed flares. Of these 18
events, 15 show detectable impulsive looptop emission. Considering that the
finite dynamic range (about a decade) of the detection introduces a strong bias
against observing comparatively weak looptop sources, we conclude that looptop
emission is a common feature of all flares. We summarize the observations of
the footpoint to looptop flux ratio and the spectral indices. We present light
curves and images of all the important newly analyzed limb flares. Whenever
possible we present results for individual pulses in multipeak flares and for
different loops for multiloop flares. We then discuss the statistics of the
fluxes and spectral indices of the looptop and footpoint sources taking into
account observational selection biases. The importance of these observations
(and those expected from the scheduled HESSI satellite with its superior
angular spectral and temporal resolution) in constraining acceleration models
and parameters is discussed briefly.Comment: 27 pages (13 embedded figures). Accepted for publication in Ap
Comparison of Hinode/XRT and RHESSI detection of hot plasma in the non-flaring solar corona
We compare observations of the non-flaring solar corona made simultaneously
with Hinode/XRT and with RHESSI. The analyzed corona is dominated by a single
active region on 12 November 2006. The comparison is made on emission measures.
We derive emission measure distributions vs temperature of the entire active
region from multifilter XRT data. We check the compatibility with the total
emission measure values estimated from the flux measured with RHESSI if the
emission come from isothermal plasma. We find that RHESSI and XRT data analyses
consistently point to the presence of a minor emission measure component
peaking at log T ~ 6.8-6.9. The discrepancy between XRT and RHESSI results is
within a factor of a few and indicates an acceptable level of
cross-consistency.Comment: 12 pages, 3 figures, Letter accepted for publicatio
- …