E-Print Archive

There are 4115 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
Turbulent pitch-angle scattering and diffusive transport of hard-X-ray producing electrons in flaring coronal loops View all abstracts by submitter

Eduard Kontar   Submitted: 2013-12-11 23:26

Recent observations from {em RHESSI} have revealed that the number of non-thermal electrons in the coronal part of a flaring loop can exceed the number of electrons required to explain the hard X-ray-emitting footpoints of the same flaring loop. Such sources cannot, therefore, be interpreted on the basis of the standard collisional transport model, in which electrons stream along the loop while losing their energy through collisions with the ambient plasma; additional physical processes, to either trap or scatter the energetic electrons, are required. Motivated by this and other observations that suggest that high energy electrons are confined to the coronal region of the source, we consider turbulent pitch angle scattering of fast electrons off low frequency magnetic fluctuations as a confinement mechanism, modeled as a spatial diffusion parallel to the mean magnetic field. In general, turbulent scattering leads to a reduction of the collisional stopping distance of non-thermal electrons along the loop and hence to an enhancement of the coronal HXR source relative to the footpoints. The variation of source size L with electron energy E becomes weaker than the quadratic behavior pertinent to collisional transport, with the slope of L(E) depending directly on the mean free path lambda again pitch angle scattering. Comparing the predictions of the model with observations, we find that lambda sim(108-109) cm for sim30 keV, less than the length of a typical flaring loop and smaller than, or comparable to, the size of the electron acceleration region.

Authors: Kontar, E. P.; Bian, N. H.; Emslie, A. G.; Vilmer, N.
Projects: RHESSI

Publication Status: accepted in ApJ
Last Modified: 2013-12-12 11:38
Go to main E-Print page  Quiescent Reconnection Rate Between Emerging Active Regions and Preexisting Field, with Associated Heating: NOAA AR 11112,  Observation of Heating by Flare-accelerated Electrons in a Solar Coronal Mass Ejection  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
Non-Stationary Fast-Driven Self-Organized Criticality in Solar Flares
Global Energetics of Solar Flares. IX. Refined Magnetic Modeling
The Solar Orbiter SPICE instrument - An extreme UV imaging spectrometer
Anisotropic Radio-Wave Scattering and the Interpretation of Solar Radio Emission Observations
Large-amplitude quasi-periodic pulsations as evidence of impulsive heating in hot transient loop systems detected in the EUV with SDO/AIA
Dynamic Evolution of Current Sheets, Ideal Tearing, Plasmoid Formation and Generalized Fractal Reconnection Scaling Relations
Characteristics of solar wind rotation
A Study of Pre-Flare Solar Coronal Magnetic Fields: Magnetic Flux Ropes
New Solar Irradiance Measurements from the Miniature X-Ray Solar Spectrometer Cubesat
MinXSS-1 CubeSat On-Orbit Pointing and Power Performance: The First Flight of the Blue Canyon Technologies XACT 3-axis Attitude Determination and Control System
The Multi-instrument (EVE-RHESSI) DEM for Solar Flares, and Implications for Nonthermal Emission
A Statistical Study of Solar Filament Eruptions That Forms High-Speed Coronal Mass Ejections
Reversed dynamo at small scales and large magnetic Prandtl number
Three-dimensional Density Structure of a Solar Coronal Streamer Observed by SOHO/LASCO and STEREO/COR2 in Quadrature
Modelling Mg II During Solar Flares, I: Partial Frequency Redistribution, Opacity, and Coronal Irradiation
The Birth of a Jet-driven Twin CME and Its Deflection from Remote Magnetic Fields
On the Origin of Solar Torsional Oscillations and Extended Solar Cycle
What Sets the Magnetic Field Strength and Cycle Period in Solar-type Stars?
Stereoscopic Observations of an Erupting Mini-filament Driven Two-Sided-Loop Jet and the Applications for Diagnosing Filament Magnetic field
Dynamic Processes of the Moreton Wave on 2014 March 29

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