Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprk11010n&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
Recent observations and theoretical considerations have pointed to a dynamic intergalactic medium, a sizable part of which is filled with magnetic fields (e.g., Kronberg et al. 2001, ApJ, 560, 178). Magnetic reconnection is an important mechanism of converting magnetic energy into heating and accelerating particles. Astrophysical plasmas often store their magnetic energy in the twists of magnetic fields and with low plasma beta (ratio of thermal to magnetic pressure), in which case it can be assumed that currents flow nearly parallel to the background magnetic field (i.e., force-free). We are investigating the onset of magnetic reconnection in such a plasma using both 2D and 3D fully kinetic particle-in- cell simulations. We use a sheet pinch, kinetic equilibrium as an initial force-free configuration (Bobrova et al. 2001, Phys. Plasmas, 8, 759). We have carried out simulations for a range of parameters, especially the current density. We have confirmed that both a short wavelength instability (Buneman mode) and a longer wavelength instability (tearing mode) may be excited (Sakai et al. 2001, Phys. Rev. E, 63, 046408). Furthermore, we find that the tearing mode is inherently unstable, regardless of whether the Buneman mode is excited. Implications for particle acceleration and heating will be presented as well as a detailed comparison with linear theories.
Colgate Stirling A.
Gary Peter S.
Li Hui
Nishimura Kazumi
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