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Paper: Investigation of Reconnection in the Solar Corona by Numerical Simulation Based on Solar-B Observations
Volume: 369, New Solar Physics with Solar-B Mission
Page: 407
Authors: Buechner, J.
Abstract: Solar-B observations are going to provide rich information which will enable a better understanding of magnetic reconnection in the solar atmosphere. So far different models exist of reconnection in three dimensions with different consequences for flare and CME triggering as well as for solar particle acceleration. Most of these models are qualitative, cartoon-like, i.e. they can neither be verified nor can they be falsified quantitatively by observations. Numerical simulation approaches are necessary to describe the nonlinear, nonlocal and ranging over extremely different scales physical processes, which are not directly observable. We discuss key aspects which have to be taken into account in order to develop appropriate forward simulation models which are able to specify the nature of solar reconnection by a direct comparison with Solar-B observations. As a starting point we discuss how to use the vector magnetic field information provided by SOT as an initial condition for the simulations. We further consider the use of the time series of SOT vector magnetic field observations to derive appropriate boundary conditions simulation models able to describe the energy input into the chromosphere and corona. Further, an appropriate coupled plasma neutral gas model is suggested, able to describe the consequences of the sub-photospheric energy input for reconnection causing electron acceleration, indirectly observable by XRT, and plasma heating, observable by EIS. Since location, triggering conditions and strength of reconnection depend on microscopic dissipation processes, we shortly review the state that appropriate transport coefficients for solar coronal conditions. Finally, we show by an example that different resistivity models might reveal completely different locations and size of three-dimensional reconnection and the corresponding electric fields in the solar corona, so that they can be verified by solar B-observations.
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