Magnetic reconnection and thermal equilibration

Abstract

When a magnetic field is forced to evolve on a time scale ${\tau }_{ev}$, as by footpoint motions driving the solar corona or non-axisymmetric instabilities in tokamaks, the magnetic field lines undergo large-scale changes in topology on a time scale approximately an order of magnitude longer than ${\tau }_{ev}$. But, the physics that allows such changes operates on a time scale eight or more orders of magnitude slower. An analogous phenomenon occurs in air. Temperature equilibration occurs on a time scale approximately an order of magnitude longer than it takes air to cross a room, ${\tau }_{ev}$, although the physical mechanism that allows temperature equilibration is approximately four orders of magnitude slower than ${\tau }_{ev}$. The use of Lagrangian coordinates allows the fundamental equations to be solved and both phenomena explained. The paradigms and presumptions of traditional theories of magnetic reconnection are so ingrained that the understanding gained from analyses using Lagrangian coordinates has been largely ignored. The theories of thermal equilibration and magnetic reconnection are developed in parallel to help readers obtain an understanding of the importance and implications of analyses using Lagrangian coordinates.

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Cited by in corpus (5)

• The rapid destruction of toroidal magnetic surfaces
• Example of exponentially enhanced magnetic reconnection driven by a spatially-bounded and laminar ideal flow
• Magnetic field evolution and reconnection in low resistivity plasmas
• Do chaotic field lines cause fast reconnection in coronal loops?
• Magnetic nulls in interacting dipolar fields