Three-dimensional magnetic reconnection in astrophysical plasmas

Abstract

Magnetic reconnection is a fundamental process in a laboratory, magnetospheric, solar and astrophysical plasma, whereby magnetic energy is converted into heat, bulk kinetic energy and fast particle energy. Its nature in two dimensions is much better understood than in three dimensions (3D), where its character is completely different and has many diverse aspects that are currently being explored. Here we focus on the magnetohydrodynamics of 3D reconnection in the plasma environment of the solar system, especially solar flares. The theory of reconnection at null points, separators and quasi-separators is described, together with accounts of numerical simulations and observations of these three types of reconnection. The distinction between separator and quasi-separator reconnection is a theoretical one that is unimportant for the observations of energy release. A new paradigm for solar flares, in which 3D reconnection plays a central role, is proposed.

37 pages, 29 figures, accepted for publication in Proceedings of The Royal Society A

References in corpus (23)

• Torus instability
• Instability of current sheets and formation of plasmoid chains
• Solar Coronal Jets: Observations, Theory, and Modeling
• Generalized Squashing Factors for Covariant Description of Magnetic Connectivity in the Solar Corona
• In situ evidence for the structure of the magnetic null in a 3D reconnection event in the Earth's magnetotail
• Observation and Modeling of Solar Jets
• Current amplification and magnetic reconnection at a 3D null point. I - Physical characteristics
• Quasi-periodic Slipping Magnetic Reconnection During an X-class Solar Flare Observed by the Solar Dynamics Observatory and Interface Region Imaging Spectrograph
• Satellite Observations of Separator Line Geometry of Three-Dimensional Magnetic Reconnection
• On the 2012 October 23 circular ribbon flare: emission features and magnetic topology
• Extreme Ultraviolet Imaging of Three-dimensional Magnetic Reconnection in a Solar Eruption
• 3D magnetic reconnection and its application to solar flares
• Flux-Rope Twist in Eruptive Flares and CMEs: due to Zipper and Main-Phase Reconnection
• Magnetohydrodynamic evolution of magnetic skeletons
• The Solar Cycle Variation of Topological Structures in the Global Solar Corona
• Slipping Magnetic Reconnection Triggering a Solar Eruption of a Triangle-flag Flux Rope
• Estimation of the magnetic flux emergence rate in the quiet Sun from Sunrise data
• Witnessing a Large-scale Slipping Magnetic Reconnection along a Dimming Channel during a Solar Flare
• Observational Analysis on the Early Evolution of a CME Flux-rope: Pre-flare reconnection and Flux-rope's Footpoint Drift
• Determination of Topology Skeleton of Magnetic Fields in a Solar Active Region
• Imaging and spectral study on the null point of a fan-spine structure during a solar flare
• Chromospheric and coronal heating and jet acceleration due to reconnection driven by flux cancellation. I. At a three-dimensional current sheet
• Is Magnetic Topology Important for Heating the Solar Atmosphere?

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