E-Print Archive

There are 4036 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
RHESSI Spectral Analysis of the 1N/M1.9 flare of 20 October 2003 View all abstracts by submitter

Hui Li   Submitted: 2004-10-14 17:44

We studied the 1N/M1.9 confined flare of 20 October 2003 observed during a joint observation program (JOP157) with emphasis on the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) X-ray spectra analysis and synthetic analysis with data from other instruments and in other wavelengths. This flare shows a long impulsive phase and four GOES 1 - 8 A X-ray peaks/plateaus implying multiple magnetic field reconnections during the flare. This results is supported by the change of hard X-ray (HXR) source at different times. Results from the RHESSI spectra analysis reveal that there were super-hot plasma bulks of up to 6.5e7 K during the impulsive phase and HXR emissions of the flare that underwent a `soft - hard - softer - harder - soft' evolution because of the multiple reconnections. Using the fitting parameters of RHESSI spectra analysis and the assumption of a `thin-target' model with a low energy cutoff of 15 keV for the power-law distribution of non-thermal electrons, we calculated the thermal and non-thermal energies stored in the flare, and showed that in most of the impulsive and gradual phase the non-thermal energy represent a small part (<15%) of the total flare energy, suggesting that the HXR emissions are of thermal feature and the energies released during several magnetic field reconnections are transported to the chromosphere mainly by thermal conduction. Factors affecting the energy estimation are discussed.

Authors: Hui Li, Arkadiusz Berlicki, and Brigitte Schmieder
Projects: None

Publication Status: Submitted to A&A
Last Modified: 2004-10-14 17:44
Go to main E-Print page  Survey on solar X-ray flares and associated coherent radio emissions  Distribution of the magnetic flux in elements of the magnetic field in active regions  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
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
Coronal Loop Seismology Using Standing Kink Oscillations With a Lookup Table
Data-Optimized Coronal Field Model: I. Proof of Concept
Coronal Bright Points
Difference of source regions between fast and slow coronal mass ejections
Invited Review: Signatures of Magnetic Flux Ropes in the Low Solar Atmosphere Observed in High Resolution
Do Kepler superflare stars really include slowly-rotating Sun-like stars ? - Results using APO 3.5m telescope spectroscopic observations and Gaia-DR2 data -
Magnetically Induced Current Piston for Generating Extreme-ultraviolet Fronts in the Solar Corona
Magnetic Field Dynamics and Varying Plasma Emission in Large-scale Coronal Loops
Nonlinear Evolution of Ion Kinetic Instabilities in the Solar Wind
What determines the X-ray intensity and duration of a solar flare?
Fast Magnetoacoustic Wave Trains with Time-dependent Drivers
Three-dimensional reconstruction of CME-driven shock-streamer interaction from radio observations: a different take on the diagnostics of coronal magnetic fields
The soft X-ray spectrometer polarimeter SolpeX
Variable emission mechanism of a Type IV radio burst
Inference of magnetic field strength and density from damped transverse coronal waves
Frequency-Distance Structure of Solar Radio Sources Observed by LOFAR
The birth of a coronal mass ejection

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