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Physics of the Solar Corona: An Introduction with Problems and Solutions
Thermal Radiation.- Hydrostatics.- Hydrodynamics.- Magnetic Fields.- Magneto-Hydrodynamics (MHD).- MHD Oscillations.- Propagating MHD Waves.- Coronal Heating.- Magnetic Reconnection.- Particle
Physics of the Solar Corona. An Introduction
Thermal Radiation.- Hydrostatics.- Hydrodynamics.- Magnetic Fields.- Magneto-Hydrodynamics (MHD).- MHD Oscillations.- Propagating MHD Waves.- Coronal Heating.- Magnetic Reconnection.- Particle
Statistics of Random Processes
The phenomenon of self-organized criticality (SOC) can be identified from many observations in the universe, by sampling statistical distributions of physical parameters, such as the distributions of
Frequency distributions and correlations of solar X-ray flare parameters
We have determined frequency distributions of flare parameters from over 12000 solar flares recorded with the Hard X-Ray Burst Spectrometer (HXRBS) on the Solar Maximum Mission (SMM) satellite. These
Time Variability of the “Quiet” Sun Observed with TRACE. II. Physical Parameters, Temperature Evolution, and Energetics of Extreme-Ultraviolet Nanoflares
We present a detailed analysis of the geometric and physical parameters of 281 EUV nanoflares, simultaneously detected with the TRACE telescope in the 171 and 195 A wavelengths. The detection and
Transverse Oscillations in Coronal Loops Observed with TRACE – II. Measurements of Geometric and Physical Parameters
We measure geometric and physical parameters oftransverse oscillations in 26 coronal loops, out of the 17 events described in Paper I by Schrijver, Aschwanden, and Title (2002). These events, lasting
Coronal Loop Oscillations Observed with the Transition Region and Coronal Explorer
We report here, for the —rst time, on spatial oscillations of coronal loops, which were detected in extreme-ultraviolet wavelengths (171 with the T ransition Region and Coronal Explorer, in the tem-
The RHESSI Imaging Concept
The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) observes solar hard X-rays and gamma-rays from 3 keV to 17 MeV with spatial resolution as high as 2.3 arc sec. Instead of focusing
Particle acceleration and kinematics in solar flares – A Synthesis of Recent Observations and Theoretical Concepts (Invited Review)
We review the physical processes of particle acceleration, injection, propagation, trapping, and energy loss in solar flare conditions. An understanding of these basic physical processes is
The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI)
RHESSI is the sixth in the NASA line of Small Explorer (SMEX) missions and the first managed in the Principal Investigator mode, where the PI is responsible for all aspects of the mission except the
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