E-Print Archive

There are 3977 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
Decametric N burst: a consequence of the interaction of two coronal mass ejections View all abstracts by submitter

Pascal Demoulin   Submitted: 2006-11-08 04:15

Radio emissions of electron beams in the solar corona and interplanetary space are tracers of the underlying magnetic configuration and of its evolution. We analyse radio observations from the Culgoora and Wind/WAVES spectrographs, in combination with SOHO/LASCO and SOHO/MDI data, to understand the origin of a type N burst originating from NOAA AR 10540 on January 20, 2004, and its relationship with type II and type III emissions. All bursts are related to the flares and the CME analysed in a previous paper (Goff et al., 2006). A very unusual feature of this event was a decametric type N burst, where a type III-like burst, drifting toward low frequencies (negative drift), changes drift first to positive, then again to negative. At metre wavelengths, i.e. heliocentric distances < 1.5 Rs, these bursts are ascribed to electron beams bouncing in a closed loop. Neither U nor N bursts are expected at decametric wavelengths because closed quasi-static loops are not thought to extend to distances >> 1.5 Rs. We take the opportunity of the good multi-instrument coverage of this event to analyse the origin of type N bursts in the high corona. Reconnection of the expanding ejecta with the magnetic structure of a previous CME, launched about 8 hours earlier, injects electrons in the same manner as with type III bursts but into open field lines having a local dip and apex. The latter shape was created by magnetic reconnection between the expanding CME and neighbouring (open) streamer field lines. This particular flux tube shape in the high corona, between 5-10 Rs, explains the observed type N burst. Since the required magnetic configuration is only a transient phenomenon formed by reconnection, severe timing and topological constraints are present to form the observed decametric N-burst. They are therefore expected to be rare features.

Authors: Demoulin, P., Klein, K.L., Goff, C.P., van Driel-Gesztelyi, L., Culhane, J.L., Mandrini, C.H., Matthews, S.A., Harra, L.K.
Projects:

Publication Status: In press, Solar Physics
Last Modified: 2006-11-23 08:56
Go to main E-Print page  The temporal evolution of coronal loops observed by GOES-SXI  Significant Results from SUMER/SOHO  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 transport and heating by torsional Alfvén waves propagating from the photosphere to the corona in the quiet Sun
A Two-Step Magnetic Reconnection in a Confined X-class Flare in Solar Active Region 12673
Lifetimes and Emergence/Decay Rates of Star Spots on Solar-type Stars Estimated by Kepler Data in Comparison with Those of Sunspots
IRIS and SDO Observations of Solar Jetlets Resulting from Network-edge Flux Cancelation
Si IV Resonance Line Emission During Solar Flares: Non-LTE, Non-equilibrium, Radiation Transfer Simulations
Study of current sheets in the wake of two crossing filaments eruption
Quasi-periodic fast propagating magnetoacoustic waves during the magnetic reconnection between solar coronal loops
Spectroscopic EUV observations of impulsive solar energetic particle event sources
CME-driven shock and Type II solar radio burst band-splitting
Signatures of magnetic reconnection at the footpoints of fan shape jets on a light bridge driven by photospheric convective motions
Drifting of the line-tied footpoints of CME flux-ropes
Three-dimensional Magnetic Reconnection Triggering an X-class Confined Flare in Active Region 12192
Oscillations accompanying a He I 10830 Å negative flare in a solar facula
The Origin of Major Solar Activity - Collisional Shearing Between Nonconjugated Polarities of Multiple Bipoles Emerging Within Active Regions
Probing the Puzzle of Behind-the-limb γ-Ray Flares: Data-driven Simulations of Magnetic Connectivity and CME-driven Shock Evolution
Transition-region explosive events produced by plasmoid instability
Flare Productivity of Major Flaring Solar Active Regions: A Time-series Study of Photospheric Magnetic Properties
Physical processes involved in the EUV "Surge" Event of 09 May 2012
Formation and Eruption of an Active Region Sigmoid. II. Magnetohydrodynamic Simulation of a Multistage Eruption
Evolution of Photospheric Vector Magnetic Field Associated with Moving Flare Ribbons As Seen By GST

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