E-Print Archive

There are 4310 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
* News 04/04/20 * The archive is using a new backend database. This has thrown up a few SQL errors in the last few days. If you have any issues please email adavey@nso.edu with either the number of eprint you are trying to edit or a link to your preprint.

Spiky Fine Structure of Type III-like Radio Bursts in Absorption View all abstracts by submitter

Gennady Chernov   Submitted: 2009-12-21 10:22

An uncommon fine structure in the radio spectrum consisting of bursts in absorption was observed with the Chinese Solar Broadband Radiospectrometer (SBRS) in the frequency range of 2.6 - 3.8 GHz during an X3.4/4B flare on 13 December 2006 in active region NOAA 10930 (S05W33). Usual fine structures in emission such as spikes, zebra stripes, and drifting fibers were observed at the peak of every new flare brightening. Within an hour at the decay phase of the event, we observed bursts consisting of spikes in absorption which pulsated periodically in frequency. Their instantaneous frequency bandwidths were found to be in the 75 MHz range. Moreover, in the strongest type III-like bursts in absorption, spikes showed stripes of the zebra-pattern (ZP), which drifted to higher frequencies. All spikes had the duration as short as down to the limit of the instrument resolution of ≈ 8 ms. The TRACE 195 Å images indicate that the magnetic reconnection at this moment occurred in the western edge of the flare loop arcade. Taking into account the presence of the reverse-drifting bursts in emission, in the course of the restoration of the magnetic structures in the corona, the acceleration of the beams of fast particles must have occurred both upward and downward at different heights. The upward beams would have been captured by the magnetic trap, where the loss-cone distribution of fast particles (responsible for the emission of continuum and ZP) were formed. Additional injection of fast particles would have filled the loss-cone later, breaking the loss-cone distribution. Therefore the generation of continuum would have been quenched at these moments, which was evidenced by the formation of bursts in absorption.

Authors: G.P. Chernov, Y.H. Yan, C.M. Tan, B. Chen, Q.J. Fu
Projects: Hinode/XRT,TRACE

Publication Status: Accepted in Solar Physics
Last Modified: 2009-12-21 12:27
Go to main E-Print page  The effect of longitudinal flow on resonantly damped kink oscillations  Kelvin-Helmholtz instability in coronal magnetic flux tubes due to azimuthal shear flows  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
Thermal-nonthermal energy partition in solar flares derived from X-ray, EUV, and bolometric observations
From Pseudostreamer Jets to Coronal Mass Ejections: Observations of the Breakout Continuum
Designing a New Coronal Magnetic Field Energy Diagnostic
A Three-Dimensional Velocity of an Erupting Prominence Prior to a Coronal Mass Ejection
Spectroscopic observations of a flare-related coronal jet
Catalog of Solar Failed Eruptions and Other Dynamic Features Registered by SDO/AIA
The non-Fourier image reconstruction method for the STIX instrument
Observation and Modeling of Solar Jets
Challenges and Advances in Modeling of the Solar Atmosphere: A White Paper of Findings and Recommendations
Non-equilibrium Flux Rope Formation by Confined Flares Preceding a Solar Coronal Mass Ejection
Radio Measurements of the Magnetic Field in the Solar Chromosphere and the Corona
A Fast, Simple, Robust Algorithm for Coronal Temperature Reconstruction
Nonlinear Alfvén Wave Model of Stellar Coronae and Winds from the Sun to M dwarfs
Possibility of Diagnostics of the Beginning of Solar Cycle 25 Based on Its Precursors at Mid-Heliolatitudes
The chromospheric component of coronal bright points. Coronal and chromospheric responses to magnetic-flux emergence
Structure of the Solar Atmosphere: A Radio Perspective
Signatures of Cross-sectional Width Modulation in Solar Spicules due to Field-aligned Flows
ALMA and IRIS Observations of the Solar Chromosphere II: Structure and Dynamics of Chromospheric Plage
ALMA and IRIS Observations of the Solar Chromosphere I: an On-Disk Type II Spicule
Evolution of a Steamer-Blowout CME as Observed by Imagers on Parker Solar Probe and the Solar Terrestrial Relations Observatory

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



© 2000-2020 Solar Physics Group - Montana State University