Mathematics – Logic
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640421l&link_type=abstract
American Astronomical Society, AAS Meeting #216, #404.21; Bulletin of the American Astronomical Society, Vol. 41, p.903
Mathematics
Logic
Scientific paper
The phenomenon of magnetic reconnection is fundamental in magnetized plasmas and of particular importance in the solar corona, where a weakly resistive single-fluid magnetohydrodynamics (MHD) description of the plasma is most appropriate. At the same time, it has long been recognized that the laminar two-dimensional (2D) uniform resistivity MHD model of magnetic reconnection is incapable of producing the fast reconnection rates inferred from solar observations. Several alternative micro-physics models have been developed to address this problem. In particular, it has been demonstrated that both the ion-electron two-fluid model and the phenomenological anomalous resistivity singe-fluid MHD model are capable of altering the structure of the 2D reconnection region to allow for reconnection rates that are sufficiently fast to be consistent with the observations. Here, we attempt to relate these two models by conducting simulations using both in a large idealized domain. To do so, we take advantage of the freedom to choose a particular form of anomalous resistivity and the existing analytic descriptions of the reconnection region within both the two-fluid and anomalous resistivity models. We then use the analytical tools to choose a form of resistivity to reproduce the characteristics of a two-fluid reconnection region and validate it in self-consistent numerical simulations. Finally, we discuss the conclusions of the study and its implications for using anomalous resistivity to model two-fluid effects in macroscopic MHD simulations of the solar corona. This research is supported by the Office of Naval Research.
Linton Mark G.
Lukin Vyacheslav
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