Abstract
Magnetic reconnection has been invoked as the energy release mechanism for solar flares and coronal mass ejections release from the sun's lower atmosphere. Theoretical models of magnetic reconnection have been traditionally developed within the frame work of magneto-hydrodynamics. However, in low density astrophysical plasmas such as in solar atmosphere, kinetic effects are expected to play a significant role. Here we have developed a kinematic theory for the prediction of CME which is a novel approach. Based on our data analysis we have assumed a general quadratic expression for the distribution function in velocity space and have looked for the complete class of self consistent magnetic fields, potential fields as well as density distributions. In our problem the occurrence of the complex roots reveal the existence of instability which can be interpreted as the CME.
Published Version
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