Physics of collisionless reconnection in a stressed X-point collapse

Details Physics of collisionless reconnection in a stressed X-point collapse Physics of collisionless reconnection in a stressed X-point collapse

2008-07-21

arxiv.org/abs/0807.3252v2

Phys. of Plasmas, 15, 102902 (2008)

Astronomy and Astrophysics

Astrophysics

Final version, accepted for publication in Physics of Plasmas

Scientific paper

10.1063/1.2999532

Recently, magnetic reconnection during collisionless, stressed, X-point collapse was studied using kinetic, 2.5D, fully electromagnetic, relativistic Particle-in-Cell numerical code [D. Tsiklauri and T. Haruki, Phys. Plasmas, 14, 112905 (2007)]. Here we finalise the investigation of this topic by addressing key outstanding physical questions. It has been established here that: (i) reconnection out-of-plane electric field at the magnetic null is generated by the electron pressure tensor off-diagonal terms, resembling to the case of tearing unstable Harris current sheet studied by the GEM reconnection challenge; (ii) For m_i / m_e >> 1 the time evolution of the reconnected flux is independent of ion-electron mass ratio; also, in the case of m_i / m_e = 1 we show that reconnection proceeds slowly as the Hall term is zero; when m_i / m_e >> 1 (i.e. the Hall term is non-zero) reconnection is fast and we conjecture that this is due to magnetic field being frozen into electron fluid, which moves significantly faster than ion fluid; (iii) within one Alfven time, somewhat less than half (40%) of the initial total (roughly magnetic) energy is converted into the kinetic energy of electrons, and somewhat more than half (60%) into kinetic energy of ions (similar to solar flare observations); (iv) in the strongly stressed X-point case, in about one Alfven time, a full isotropy in all three spatial directions of the velocity distribution is seen for super-thermal electrons (also commensurate to solar flare observations).

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