Recent results on magnetic plasma turbulence
AIP Conference Proceedings
American Institute of Physics (AIP)
This is the final version of the article. Available from the American Institute of Physics via the DOI in this record.
Magnetic plasma turbulence is observed over a broad range of scales in the solar wind. We discuss the results of high-resolution numerical simulations of magnetohydrodynamic (MHD) turbulence that models plasma motion at large scales and the results of numerical simulations of kinetic-Alfvén turbulence that models plasma motion at small, sub-proton scales. The simulations, with numerical resolutions up to 20483 mesh points in the MHD case and 5123 points in kinetic-Alfvén case and statistics accumulated over 30 to 150 eddy turnover times, constitute, to the best of our knowledge, the largest statistical sample of steadily driven three dimensional MHD and kinetic-Alfvén turbulence to date.
This work was supported by the NSF/DoE partnership grant NSF-ATM-1003451 at the University of New Hampshire, the NSF sponsored Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas at the University of Chicago and the University of Wisconsin - Madison, the US DoE awards DE-FG02- 07ER54932, DE-SC0003888, DE-SC0001794, the NSF grants PHY-0903872 and AGS-1003451, and the DoE INCITE 2010 Award. This research used resources of the Argonne Leadership Computing Facility at Argonne National Laboratory, supported by the DoE Office of Science under contract DE-AC02-06CH11357. The studies were also supported by advanced computing resources provided by the NSF XSEDE allocation TG-PHY110016 at the National Institute for Computational Sciences and the PADS resource (NSF grant OCI-0821678) at the Computation Institute, a joint institute of Argonne National Laboratory and the University of Chicago.
AIP Conference Proceedings, 2013, Vol. 1539, pp. 135 - 138