Two-Dimensional MHD Simulation of Chromospheric Evaporation
Driven by Magnetic Reconnection in Solar Flares
The thermal energy driving the evaporation is first supplied from the coronal
magnetic field through the magnetic reconnection mechanism
and is transported into the chromosphere by heat conduction.
Nonlinear anisotropic heat conduction
and radiative cooling of optically-thin plasma
are taken into account.
The results show that temperature distribution is similar to the
cusp-like structure of long-duration-event (LDE) flares
observed by the soft X-ray telescope aboard Yohkoh satellite.
Three-Dimensional MHD Simulation of Magneto-rotational Instability
Discovery of Reconnection Inflow of a Solar Flare
Scaling Law of Flare T vs. EM
Discovery of Sub-Second-Time-Scale Propagation of a Non-Thermal Source
by Nobeyama Radioheligoraph
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