E-Print Archive

There are 3897 abstracts currently viewable.


Search:

Advanced Search
Options
Main Page Add New E-Print Submitter
Information
Feedback
News Help/FAQ About Preferences
Manage Key Phrase
Notification
Magnetic reconnection from a multiscale instability cascade View all abstracts by submitter

Paul Bellan   Submitted: 2012-02-15 21:51

Magnetic reconnection, the process whereby magnetic field lines breakand then reconnect to form a different topology, underlies criticaldynamics of magnetically confined plasmas in both natura1, andthe laboratory. Magnetic reconnection involves localizeddiffusion of the magnetic field across plasma, yet observedreconnection rates are typically much higher than can be accounted forusing classical electrical resistivity. It is generally proposedthat the field diffusion underlying fast reconnection results insteadfrom some combination of non-magnetohydrodynamic processes that becomeimportant on the 'microscopic' scale of the ion Larmor radius or theion skin depth. A recent laboratory experiment11 demonstrated atransition from slow to fast magnetic reconnection when a currentchannel narrowed to a microscopic scale, but did not address how amacroscopic magnetohydrodynamic system accesses the microscale. Recenttheoretical models and numerical simulations suggest that amacroscopic, two-dimensional magnetohydrodynamic current sheet mightdo this through a sequence of repetitive tearing and thinning intotwo-dimensional magnetized plasma structures having successively finerscales. Here we report observations demonstrating a cascade ofinstabilities from a distinct, macroscopic-scale magnetohydrodynamicinstability to a distinct, microscopic-scale (ion skin depth)instability associated with fast magnetic reconnection. Theseobservations resolve the full three-dimensional dynamics and giveinsight into the frequently impulsive nature of reconnection in spaceand laboratory plasmas.

Authors: Auna L. Moser & Paul M. Bellan
Projects: None

Publication Status: published as a Nature Letter, February 16, 2012, online on Feb 15
Last Modified: 2012-02-17 08:42
Go to main E-Print page  On the Role of the Background Overlying Magnetic Field in Solar 
Eruptions  Speeds and arrival times of solar transients approximated by self-similar expanding circular fronts  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Key
Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Computation of Relative Magnetic Helicity in Spherical Coordinates
Some characteristics of the GLE on 10 September 2017
Quasi-periodic Pulsations in a Solar Microflare
Homologous large-amplitude Nonlinear fast-mode Magnetosonic Waves Driven by Recurrent Coronal Jets
EUV Waves Driven by Sudden Expansion of Transequatorial Loops Caused by Solar Coronal Jets
Dispersively formed quasi-periodic fast magnetosonic wavefronts due to the eruption of a nearby mini-filament
Mini-filament Eruptions Triggering Confined Solar Flares Observed by ONSET and SDO
LOFAR observations of fine spectral structure dynamics in type IIIb radio bursts
Critical magnetic field strengths for solar coronal plumes in quiet regions and coronal holes?
Does Nearby Open Flux Affect the Eruptivity of Solar Active Regions?
Cyclic Changes of the Sun's Seismic Radius
Onset of Photospheric Impacts and Helioseismic Waves in X9.3 Solar Flare of September 6, 2017
Solar Cycle Variations of Rotation and Asphericity in the Near-Surface Shear Layer
Solar coronal loop dynamics near the null point above active region NOAA 2666
Energetics of small electron acceleration episodes in the solar corona from radio noise storm observations
The origin of the modulation of the radio emission from the solar corona by a fast magnetoacoustic wave
Indirect solar wind measurements using archival cometary tail observations
Helium abundance and speed difference between helium ions and protons in the solar wind from coronal holes, active regions, and quiet Sun
Always a Farm Boy
Effect of transport coefficients on excitation of flare-induced standing slow-mode waves in coronal loops

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey



© 2003 Solar Physics Group - Montana State University