E-Print Archive

There are 4053 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Diagnostics of electron beam properties from the simultaneous hard X-ray and microwave emission in the 10 March 2001 flare View all abstracts by submitter

Valentina Zharkova   Submitted: 2011-05-23 08:56

Simultaneous simulation of HXR and MW emission with the same populations ofelectrons is still a great challenge for interpretation of observations in realevents. In this paper we apply the FP kinetic model of precipitation ofelectron beam with energy range from 12 keV to 1.2 MeV to the interpretation ofX-ray and microwave emissions observed in the flare of 10 March 2001. Methods.The theoretical HXR and MW emissions were calculated by using the distributionfunctions of electron beams found by solving time-dependent Fokker-Planckapproach in a converging magnetic field (Zharkova at al., 2010; Kuznetsov andZharkova, 2010) for anisotropic scattering of beam electrons on the ambientparticles in Coloumb collisions and Ohmic losses. The simultaneous observed HXRphoton spectra and frequency distribution of MW emission and polarization werefit by those simulated from FP models which include the effects of electricfield induced by beam electrons and precipitation into a converging magneticloop. Magnetic field strengths in the footpoints on the photosphere wereupdated with newly calibrated SOHO/MDI data. The observed HXR energy spectrumabove 10 keV is shown to be a double power law which was fit precisely by thephoton HXR spectrum simulated for the model including the self-induced electricfield but without magnetic convergence. The MW emission simulated for differentmodels of electron precipitation revealed a better fit to the observeddistribution at higher frequencies for the models combining collisions andelectric field effects with a moderate magnetic field convergence of 2. The MWsimulations were able to reproduce closely the main features of the MW emissionobserved at higher frequencies.

Authors: Zharkova, V.V., Meshalkina, N.S., Kashapova, L.K., Kuznetsov, A.A. and Altyntsev A.T.
Projects: RHESSI

Publication Status: Astronomy and Astrophysics, in press
Last Modified: 2011-05-24 09:44
Go to main E-Print page  Radio emission of the Quiet Sun and Active Regions (Invited review)  Successive merging of plasmoids and fragmentation in a flare current sheet and their X-ray and radio signatures  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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
Linear waves in a non-equilibrium ionisation partially ionised plasma
How Many Twists Do Solar Coronal Jets Release?
Different Signatures of Chromospheric Evaporation in Two Solar Flares Observed with IRIS
The Physical Nature of Spiral Wave Patterns in Sunspots
Predicting Solar Flares Using a Long Short-Term Memory Network
Coronal loop transverse oscillations excited by different driver frequencies
Solar Center-Limb Variation of the Strengths of Spectral Lines: Classification and Interpretation of Observed Trends
The plasmoid instability in a confined solar flare
High-frequency dynamics of active region moss as observed by IRIS
Extreme-ultraviolet Late Phase Caused by Magnetic Reconnection over Quadrupolar Magnetic Configuration in a Solar Flare
Two-step evolution of a rising flux rope resulting in a confined solar flare
Why torus-unstable solar filaments experience failed eruption?
The Magnetic Properties of Heating Events on High-Temperature Active Region Loops
Pulse-beam heating of deep atmospheric layers, their oscillations and shocks modulating the flare reconnection
A potential magnetic field calculator for solar physics applications using staggered grids
E and B polarizations from inhomogeneous and solar surface turbulence
Oscillations Accompanying a He I 10830 Å Negative Fare in a Solar Facula II. Response of the Transition Region and Corona
Flare reconnection-driven magnetic field and Lorentz force variations at the Sun's surface
Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?
Impacts On Proton Fluxes Observed During Different Interplanetary Conditions

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