Impulsive Magnetic Reconnection in the Earth's Magnetotail and the Solar Corona

By Ashis Bhattacharjee. 2004

158 citations recorded by the source corpus.

▪ Abstract Impulsive reconnection dynamics is characterized not only by fast growth but also by a sudden change in the time derivative of the growth rate. I review recent developments in the theory and simulation of forced impulsive reconnection based on the equations of resistive and Hall magnetohydrodynamics (MHD). Impulsive reconnection can be realized in resistive as well as Hall MHD by the imposition of suitable boundary conditions. However, compared with resistive MHD, Hall MHD reconnection is distinguished by qualitatively different magnetic field and electron and ion signatures in the reconnection layer. Furthermore, nonlinear reconnection rates in Hall MHD are weakly dependent on the Lundquist number. I discuss applications of the physics of impulsive reconnection to substorms in the Earth's magnetotail and solar flares.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/65ada977b64aa8ffca2f3723ae1d2da19274d9bd

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Citations in the corpus

Wave turbulence in incompressible Hall magnetohydrodynamics (2006, methodology): “We decompose the inviscid nonlinear Hall MHD equations ( 14 )–(15) on the complex helicity decomposition introduced in the previous section.”
Magnetic Reconnection in Astrophysical and (2009, background): “An earlier ARAA review (Bhattacharjee 2004) emphasizes impulsive reconnection in the collisionless regime.”
NUMERICAL TESTS OF FAST RECONNECTION IN WEAKLY STOCHASTIC MAGNETIC FIELDS (2009, background): “This is a vital question for many areas of astrophysics (see Biskamp 2000; Priest & Forbes 2000; Bhattacharjee 2004; Zweibel & Yamada 2009).”
Ultraviolet spectroscopy of the extended solar corona (2006, background): “Existing models of current sheets do not yet reliably predict the reconnection rate or the fractions of the dissipated energy that emerge as heat, kinetic energy, and nonthermal particles, but considerable theoretical progress is being made (e.g., Priest & Forbes 2000; Bhattacharjee 2004).”
On Solving the Coronal Heating Problem (2005, background): “Recent studies suggest that collisionless effects may be extremely important for reconnection (e.g., Birn et al. 2001; Bhattacharjee, 2004).”
Modelling Quasi-Periodic Pulsations in Solar and Stellar Flares (2018, background): “Sweet–Parker and Petschek cannot account for the time evolution of the reconnection rate.”
Observation of energetic electrons within magnetic islands (2008, background): “The observed structures are identified as magnetic islands on the basis of the following criteria: (1) bipolar Bz involving a sign change (Fig.”