Pseudo-reconnection in MHD numerical simulation.

Details Pseudo-reconnection in MHD numerical simulation. Pseudo-reconnection in MHD numerical simulation.

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000chsbu..45..798c&link_type=abstract

Chin. Sci. Bull., Vol. 45, No. 9, p. 798 - 801

Physics

13

Plasma: Magnetic Reconnection, Magnetohydrodynamics: Numerical Simulations, Magnetohydrodynamics: Solar Physics

Scientific paper

Magnetic reconnection is now regarded to play an essential role in space plasma and laboratory or astrophysical plasma. For the Sun, it is widely used to explain many solar active phenomena, such as solar flares, X-ray jets and coronal heating. With some approximation, the magnetic reconnection can be described by resistive MHD equations. Due to the high nonlinearity of the equations, it is difficult to analytically solve them, and only a few special solutions have been found. Numerical simulation provides a powerful approach in this aspect, and has made much progress. However, numerical simulation may sometimes introduce unphysical results, for example, numerical instability. For the first time, this note reports a class of pseudo-reconnections caused by numerical resistivity in a shifted mesh system.

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