Magnetic reconnection is a topological rearrangement of magnetic field that occurs on time scales much faster than the global magnetic diffusion time. Since the field lines break on microscopic scales but energy is stored and the field is driven on macroscopic scales, reconnection is an inherently multi-scale process that often involves both magnetohydrodynamic (MHD) and kinetic phenomena. In this article, we begin with the MHD point of view and then describe the dynamics and energetics of reconnection using a two-fluid formulation. We also focus on the respective roles of global and local processes and how they are coupled. We conclude that the triggers for reconnection are mostly global, that the key energy conversion and dissipation processes are either local or global, and that the presence of a continuum of scales coupled from microscopic to macroscopic may be the most likely path to fast reconnection.
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http://dx.doi.org/10.1098/rspa.2016.0479 | DOI Listing |
Acta Biomater
January 2025
School of Life Sciences, Keele University, Staffordshire, UK. Electronic address:
The ability to control the growth and orientation of neurites over long distances has significant implications for regenerative therapies and the development of physiologically relevant brain tissue models. In this study, the forces generated on magnetic nanoparticles internalised within intracellular endosomes are used to direct the orientation of neuronal outgrowth in cell cultures. Following differentiation, neurite orientation was observed after 3 days application of magnetic forces to human neuroblastoma (SH-SY5Y) cells, and after 4 days application to rat cortical primary neurons.
View Article and Find Full Text PDFSci Rep
December 2024
LATMOS-IPSL-CNRS, 75252, Paris, France.
The ground-based solar telescope THEMIS performed several observations of Mercury's sodium exosphere in years 2011-2013, when the MESSENGER spacecraft was orbiting around the planet. Typical two-peak exospheric patterns were frequently identified. In previous studies, some specific cases of THEMIS Na two-peak observations were characterized and related to IMF conditions, during specific extreme cases, in the occasion of CME arrival.
View Article and Find Full Text PDFSci Rep
December 2024
Mathematics, KU Leuven, Celestijnenlaan 200B, Leuven, Belgium.
The formation of a S-shaped filament was investigated to determine if and how magnetoacoustic waves in the solar corona can trigger filament excitation. The study investigated how magnetoacoustic waves interact with two magnetic null points in the solar corona. Since the solar corona has a complex magnetic field structure, it is expected that magnetic structures are predominantly responsible for the occurrence of coronal events.
View Article and Find Full Text PDFEarth Planets Space
December 2024
Department of Physics and Engineering Physics, University of Saskatchewan, Saskatoon, SK Canada.
Unlabelled: The lunar environment heliospheric X-ray imager (LEXI) and solar wind-magnetosphere-ionosphere link explorer (SMILE) will observe the magnetopause motion in soft X-rays to understand dayside reconnection modes as a function of solar wind conditions after their respective launches in the near future. To support their successful science mission, we investigate the relationship between the magnetopause position and the dayside reconnection rate by utilizing super dual auroral radar network (SuperDARN) observations and widely used empirical models of magnetopause position (Shue et al. in J Geophys Res 103:17691-17700.
View Article and Find Full Text PDFPhys Rev E
November 2024
School of Physical and Chemical Sciences, Queen Mary University of London, London E1 4NS, United Kingdom and Space Weather Technology, Research and Education Center (SWx-TREC), University of Colorado, Boulder, Colorado 80309, USA.
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