E-Print Archive

There are 2921 abstracts currently viewable.
There is a problem with some abstracts that became corrupted following database issues. These will be restored as soon as possible.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
X-ray sources and magnetic reconnection in the X3.9 flare of 2003 November 3 View all abstracts by submitter

Astrid Veronig   Submitted: 2005-09-30 06:16

Recent RHESSI observations indicate an apparent altitude decrease of flare X-ray loop-top (LT) sources before changing to the commonly observed upward growth of the flare loop system. We performed a detailed study of the LT altitude decrease for one well observed flare in order to find further hints on the physics of this phenomenon and how it is related to the magnetic reconnection process in solar flares. RHESSI X-ray source motions in the 2003 November 3, X3.9 flare are studied together with complementary data from SXI, EIT, and Kanzelhohe H α . We particularly concentrate on the apparent altitude decrease of the RHESSI X-ray LT source early in the flare and combine kinematical and X-ray spectral analysis. Furthermore, we present simulations from a magnetic collapsing trap model embedded in a standard 2-D magnetic reconnection model of solar flares. We find that at higher photon energies the LT source is located at higher altitudes and shows higher downward velocities than at lower energies. The mean downward velocities range from 14 km s-1 in the RHESSI 10--15~keV energy band to 45 km s-1 in the 25--30 keV band. For this flare, the LT altitude decrease was also observed by the SXI instrument with a mean speed of 12 km s-1. RHESSI spectra indicate that during the time of LT altitude decrease the emission of the LT source is thermal bremsstrahlung from a ``superhot'' plasma with temperatures increasing from 35 MK to 45 MK and densities of the order of 1010 cm-3. The temperature does not significantly increase after this early (pre-impulsive superhot LT) phase, whereas the LT densities increase to a peak value of (3--4)cdot 1011 cm-3.} Modeling of a collapsing magnetic trap embedded in a standard 2D magnetic reconnection model can reproduce the key observational findings in case that the observed emission is thermal bremsstrahlung from the hot LT plasma. This is in accordance with the evaluated RHESSI spectra for this flare.

Authors: A.M. Veronig, M. Karlicky, B. Vrsnak, M. Temmer, J. Magdalenic, B.R. Dennis, W. Otruba, W. Poetzi
Projects: RHESSI

Publication Status: A&A (accepted)
Last Modified: 2005-09-30 06:16
Go to main E-Print page  Multiwavelength Analysis of a Solar Flare on 2002 April 15  Multi-wavelength study of coronal waves associated with the CME-flare event of 03 November 2003  Edit Entry  Download Preprint  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
Fast Magnetic Twister and Plasma Perturbations in a 3-D Coronal Arcade
Evidence of Electron Acceleration around the Reconnection X-point in a Solar Flare
On the helicity of open magnetic fields
The coronal energy input from magnetic braiding
Connecting speeds, directions and arrival times of 22 coronal mass ejections from the Sun to 1 AU
A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. III. Catastrophe of the Eruptive Filament in a Magnetic Null Point and Formation of an Opposite-Handedness CME
On the variation of solar flare coronal X-ray source sizes with energy
Observational Evidence of Torus Instability as Trigger Mechanism for Coronal Mass Ejections: The 2011 August 4 Filament Eruption
Fast magnetohydrodynamic oscillation of longitudinally inhomogeneous prominence threads: an analogue with quantum harmonic oscillator
The Low-High-Low Trend of Type III Radio Burst Starting Frequencies and Solar Flare Hard X-rays
Observations of a Hybrid Double-Streamer/Pseudostreamer in the Solar Corona
A Chain of Winking (Oscillating) Filaments Triggered by an Invisible Extreme-Ultraviolet Wave
Coronal Condensation in Funnel Prominences as Return Flows of the Chromosphere-Corona Mass Cycle
Nonlinear Force-Free Field Extrapolation of a Coronal Magnetic Flux Rope Supporting a Large-Scale Filament from Photospheric Vector Magnetogram
Determination of the cross-field density structuring in coronal waveguides using the damping of transverse waves
RATAN-600 Observations of Small Scale Structures with High Spectral Resolution
Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review)
Anomalous Expansion of Coronal Mass Ejections during Solar Cycle 24 and its Space Weather Implications
The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs - Space-weather HMI Active Region Patches
Compound Effect of Alfv?n Waves and Ion-cyclotron Waves on Heating/Acceleration of Minor Ions via the Pickup Process

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