E-Print Archive

There are 4354 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
Budget of energetic electrons during solar flares in the framework of magnetic reconnection View all abstracts by submitter

Gottfried Mann   Submitted: 2011-03-29 07:49

Among other things, solar flares are accompanied by the production ofenergetic electrons as seen in the nonthermal radio and X-rayradiation of the Sun. Observations of the RHESSI satellite show that1032-1036 nonthermal electrons are produced per secondduring flares. They are related to an energy flux in the range1018-1022 W. These electrons play an important role, sincethey carry a substantial part of the energy released during a flare.In which way so many electrons are accelerated up to high energiesduring a fraction of a second is still an open question. By means ofradio and hard X-ray data, we investigate under which conditions thisacceleration happens in the corona. The flare is considered in theframework of magnetic reconnection. The conditions in the accelerationregion in the corona are deduced by using the conservation of thetotal electron number and energy. In the inflow region of the magneticreconnection site, there are typical electron number densities ofabout 2.07 x 109 cm-3 and magnetic fields ofabout 46 G.These are regions with high Alfvén speeds of about 2200 km s-1. Then,sufficient energetic electrons (as required by the RHESSIobservations) are only generated if the plasma inflow towards thereconnection site has Alfvén-Mach numbers in the range 0.1-1, whichcan lead to a super-Alfvénic outflow with speeds up to 3100 kms-1.

Authors: G. Mann and A. Warmuth
Projects: RHESSI

Publication Status: Published in Astron. and Astrophys.
Last Modified: 2011-03-30 08:57
Go to main E-Print page  TomograPy: A Fast, Instrument-Independent, Solar Tomography Software  Nonlinear long-wavelength tortional
Alfvén waves  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
Energy budget of plasma motions, heating, and electron acceleration in a three-loop solar flare
Space weather: the solar perspective - an update to Schwenn (2006)
Mixed properties of slow magnetoacoustic and entropy waves in a plasma with heating/cooling misbalance
The morphology of average solar flare time profiles from observations of the Sun's lower atmosphere
Indications of stellar coronal mass ejections through coronal dimmings
Could switchbacks originate in the lower solar atmosphere? II. Propagation of switchbacks in the solar corona
Solar large-scale magnetic field and cycle patterns in solar dynamo
Three-dimensional magnetic reconnection in astrophysical plasmas
Energy partition in a confined flare with an extreme-ultraviolet late phase
Alfvén wave heating in partially ionized thin threads of solar prominences
He I 10830 Dimming During Solar Flares, I: The Crucial Role of Non-Thermal Collisional Ionisations
Separating aa-index into Solar and Hale Cycle Related Components Using Principal Component Analysis
Inward Propagating Plasma Parcels in the Solar Corona: Models with Aerodynamic Drag, Ablation, and Snowplow Accretion
Energetics and 3-D Structure of Elementary Events in Solar Coronal Heating
Stellar Superflares Observed Simultaneously with Kepler and XMM-Newton
Medium-term predictions of F10.7 and F30 cm solar radio flux with the adaptive Kalman filter
Resonances in a Coronal Loop Driven by Torsional Alfvén Waves Propagating from the Photosphere
Effects of external flow on resonant absorption of coronal loop kink oscillations driven by an external fast wave: Selective excitation problem
Emerging Dimming as Coronal Heating Episodes
Proxy-Based Prediction of Solar Extreme Ultraviolet Emission using Deep Learning

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