E-Print Archive

There are 3715 abstracts currently viewable.


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. Karlický, 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
Microflare Heating of a Solar Active Region Observed with NuSTAR, Hinode/XRT, and SDO/AIA
Successive Two-sided loop Jets Caused by Magnetic Reconnection between Two adjacent Filamentary Threads
Solar plasma radio emission in the presence of imbalanced turbulence of kinetic-scale Alfvén waves
Spatial Offsets in Flare-CME Current Sheets
Magnetic Flux Rope Shredding by a Hyperbolic Flux Tube: The Detrimental Effects of Magnetic Topology on Solar Eruptions
Observational Study on the Fine Structure and Dynamics of a Solar Jet. I. Energy Build-Up Process around a Satellite Spot.
Coronal Holes and Open Magnetic Flux over Cycles 23 and 24
Gradual Solar Coronal Dimming and Evolution of Coronal Mass Ejection in the Early Phase
Elongation of Flare Ribbons
The eruption of a small-scale emerging flux rope as the driver of an M-class flare and a coronal mass ejection
Magnetic Flux Cancelation as the Origin of Solar Quiet Region Pre-Jet Minifilaments
Three-dimensional oscillatory magnetic reconnection
Quasi-Periodic Radio Bursts Associated with Fast-mode Waves near a Magnetic Null Point
Onset of a Large Ejective Solar Eruption from a Typical Coronal-Jet-Base Field Configuration
Heating of an erupting prominence associated with a solar coronal mass ejection on 2012 January 27
New Evidence that Magnetoconvection Drives Solar-Stellar Coronal Heating
Beam electrons as a source of Hα flare ribbons
A hybrid supervised/unsupervised machine learning approach to solar flare prediction
Magnetohydrodynamic Simulations for Studying Solar Flare Trigger Mechanism
Sunspot Light Walls Suppressed by Nearby Brightenings

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