Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm31a1716z&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SM31A-1716
Astronomy and Astrophysics
Astrophysics
7827 Kinetic And Mhd Theory, 7833 Mathematical And Numerical Techniques (0500, 3200), 7835 Magnetic Reconnection (2723, 7526), 7839 Nonlinear Phenomena (4400, 6944), 7899 General Or Miscellaneous
Scientific paper
Magnetic reconnection is a driver of explosive events in space- and astrophysical plasmas. It also plays a role in high-energy astrophysical settings such as pulsar winds and magnetar flares, where plasmas are composed of relativistic electrons and positrons. Kinetic-scale properties of relativistic magnetic reconnection in these environments have been recently investigated by PIC simulations. In addition, a good relativistic MHD model is needed in order to model further large-scale problems. However, due to the extreme complexity of the equation system, the number of MHD studies has been quite limited. We have recently developed a relativistic multi-fluid code to study large-scale reconnection problems. We consider a symmetric two-fluid system (positron fluid and electron fluid) and introduce an inter-species friction term to represent an effective resistivity. With a spatially localized resistivity profile, we successfully simulated magnetic reconnection in a relativistic two-fluid system. In this paper we will present the nonlinear, large- scale, long-term evolutions, and parameter dependencies (e.g. reconnection rate vs inflow energy composition) of the relativistic MHD reconnection system.
Hesse Matthias
Klimas Alex
Zenitani Seiji
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