Particle distributions in collisionless magnetic reconnection: An implicit PIC (Particle-In-Cell) description

Conference · Wed Oct 03 04:00:00 EDT 1990

OSTI ID:6416676

Hewett, D W; Francis, G E; Max, C E

Evidence from magnetospheric and solar flare research supports the belief that collisionless magnetic reconnection can proceed on the Alfven-wave crossing timescale. Reconnection behavior that occurs this rapidly in collisionless plasmas is not well understood because underlying mechanisms depend on the details of the ion and electron distributions in the vicinity of the emerging X-points. We use the direct implicit Particle-In Cell (PIC) code AVANTI to study the details of these distributions as they evolve in the self-consistent E and B fields of magnetic reconnection. We first consider a new simple neutral sheet model and see reconnection that proceeds much more rapidly than reconnection from the Harris equilibrium. We observe rapid movement of the current-carrying electrons away from the emerging X-point. Later in time an oscillation of the trapped magnetic flux is found, superimposed upon continued linear growth due to plasma inflow at the ion sound speed. The addition of a current-aligned (east-west direction in the magnetosphere) and a normal (north-south in the magnetosphere) B field widen the scope of the our studies. 10 refs., 9 figs.

• Research Organization: Lawrence Livermore National Lab., CA (USA)
• Sponsoring Organization: DOE/DP
• DOE Contract Number: W-7405-ENG-48
• OSTI ID: 6416676
• Report Number(s): UCRL-JC-104418-Rev.1; CONF-9006220--5-Rev.1; ON: DE91002786
• Country of Publication: United States
• Language: English

Related Subjects

640201* -- Atmospheric Physics-- Auroral
Ionospheric
& Magetospheric Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ALFVEN WAVES
COLLISIONLESS PLASMA
DISTRIBUTION FUNCTIONS
EARTH ATMOSPHERE
EARTH MAGNETOSPHERE
FLUID MECHANICS
FUNCTIONS
HYDRODYNAMICS
HYDROMAGNETIC WAVES
MAGNETIC RECONNECTION
MAGNETOHYDRODYNAMICS
MECHANICS
PLASMA
PLASMA SIMULATION
SIMULATION
SOLAR ACTIVITY
SOLAR FLARES