E-Print Archive

There are 4524 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 topologies: where will reconnection occur ? View all abstracts by submitter

Pascal Demoulin   Submitted: 2005-10-12 06:05

The energy needed to power flares is thought to come from the coronal magnetic field. However, such energy release is efficient only at very small scales. Magnetic configurations with a complex topology, i.e. with separatrices, are the most obvious configurations where current layers can spontaneously form. 3-D magnetic configurations have a variety of magnetic topologies not suspected before. If the photospheric field is described by an ensemble of magnetic charges, separated by flux-free regions, a complete topological description of the associated potential field is provided by the skeleton formed by the null points, spines, fans and separators. In order to better match the observed photospheric magnetograms, the magnetic charges can be set below the photosphere; then an extra topological element can appear, so-called bald patches with associated separatrices. In several flaring configurations the computed separatrices allows to understand the localization of the flare ribbons in the framework of magnetic reconnection. However, this view is too restrictive taking into account the variety of observed solar flaring configurations. Indeed ``quasi-separatrix layers'' (QSLs), which are regions where there is a drastic change in field-line linkage, generalize the definition of separatrices for magnetic fields extending in the full volume (photosphere and corona). The concept of ``hyperbolic flux tube'' (HFT) also generalizes the concept of separator. These studies indeed teach us that coronal magnetic reconnection occurs in a broader variety of magnetic configurations than traditionally thought, and this variety is reviewed.

Authors: Demoulin, P.
Projects: None

Publication Status: ESA publication, in press
Last Modified: 2005-10-12 06:05
Go to main E-Print page  Particle simulation of plasma heating by large amplitude shear Alfven wave through its transverse modulation in collisionless plasmas  Compton backscattered and primary X-rays from solar flares: angle dependent Green's function correction for photospheric albedo  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
Coronal seismology by slow waves in non-adiabatic conditions
Exploring the Ideal MHD Quasi-Modes of a Plasma Interface with a Thick Nonuniform Transition
Changes of Magnetic Energy and Helicity in Solar Active Regions from Major Flares
Spectroscopic and Imaging Observations of Spatially Extended Magnetic Reconnection in the Splitting of a Solar Filament Structure
The Universality of Power Law Slopes in the Solar Photosphere and Transition Region Observed with HMI and IRIS
Turbulence and Anomalous Resistivity inside Near-Earth Magnetic Clouds
On the specific energy and pressure in near-Earth magnetic clouds
Solar Energetic Particle Event Associated with the 2012 July 23 Extreme Solar Storm
Investigation of Energetic Particle Release Using Multi-point Imaging and In Situ Observations
Shock Properties and Associated Characteristics of Solar Energetic Particles in the 2017 September 10 GLE event
Dimensionality of Solar Magnetic Reconnection
Microwave Perspective on Magnetic Breakout Eruption
Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave
Multi-spacecraft Observations of the Coronal and Interplanetary Evolution of a Solar Eruption Associated with Two Active Regions
Sun-to-Earth Characteristics of the 2012 July 12 Coronal Mass Ejection and Associated Geo-effectiveness
The effect of nanoflare flows on EUV spectral lines
On some features of the solar proton event on 2021 October 28 GLE73
The role and contribution of magnetic fields, characterized via their magnetic flux, to the statistical structuring of the solar atmosphere
Do periods of decayless kink oscillations of solar coronal loops depend on noise?
Automatic detection technique for solar filament oscillations in GONG data

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



© 2000-2020 Solar Physics Group - Montana State University