E-Print Archive

There are 4620 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Statistical study of Type III bursts and associated HXR emissions View all abstracts by submitter

Nicole Vilmer   Submitted: 2023-03-28 03:06

Context. Flare-accelerated electrons may produce closely temporarily related hard X-ray emission while interacting with the dense solar atmosphere and radio type III bursts when propagating from the low corona to the interplanetary medium. The link between these emissions has been studied in previous studies. We present here new results on the correlation between the number and spectrum of HXR producing electrons and the type III characteristics (flux, starting frequency). Aims. The aim of this study is to extend the results from previous statistical studies of radio type III bursts and associated HXR emissions: in particular what kind of correlation, if any, exists between the HXR emitting electron numbers and the radio flux? Are there any correlations between the electron numbers or energy spectra deduced from associated HXR emissions and type III starting (stopping) frequencies? Methods. This study is based on thirteen years of data between 2002 and 2014. We shortlisted ~ 200 events with close temporal association between HXR emissions and radio type III bursts in the 450-150 MHz range. We used X-ray flare observations from RHESSI and FERMI/GBM to calculate the number of electrons giving rise to the observed X-ray flux and observations from the Nanšay Radioheliograph to calculate the peak radio flux at different frequencies in the 450-150 MHz range. Under the assumption of thick-target emissions, the number of HXR producing electrons and their energy spectra were computed . The correlation between electron numbers, power-law indices and the peak radio fluxes at different frequencies were analysed as well as potential correlations between electron numbers and starting frequency of the radio burst. Bootstrap analysis for the correlation coeffcients was performed to quantify the statistical significance of the fit. Results. The correlation between the number of HXR electrons and the peak flux of the type III emission decreases with increasing frequency. This correlation is larger when considering electron number above 20 keV rather than electron number above 10 keV. A weak anticorrelation is also found between the absolute value of the electron spectral index and the peak radio flux at 228 MHz. A rough correlation is found between the HXR producing electron number above 20 keV and the type III starting frequency. This correlation is smaller if the electron number above 10 keV is considered. All the results are discussed in the framework of results from previous studies and in the context of numerical simulations of bump-in-tail instabilities and subsequent radio emissions.

Authors: Tomin James & Nicole Vilmer
Projects: Wind

Publication Status: Astronomy and Astrophysics in press
Last Modified: 2023-03-29 14:54
Go to main E-Print page  Solar Radio Spikes and Type IIIb Striae Manifestations of Sub-second Electron Acceleration Triggered by a Coronal Mass Ejection  On orbit performance of the solar flare trigger for the Hinode EUV Imaging Spectrometer  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
High-altitude Spider-type Prominence above the Magnetic Null Point
Non-Neutralized Electric Currents as a Proxy for Eruptive Activity in Solar Active Regions
Formation and Dynamics in an Observed Preeruptive Filament
Unveiling the spectacular over 24-hour flare of star CD-36 3202
The centroid speed as a characteristic of the group speed of solar coronal fast magnetoacoustic wave trains
Coronal dimmings as indicators of early CME propagation direction
A Chromatic Treatment of Linear Polarization in the Solar Corona at the 2023 Total Solar Eclipse
MinXSS-2 CubeSat mission overview: Improvements from the successful MinXSS-1 mission
Small Satellite Mission Concepts for Space Weather Research and as Pathfinders for Operations
Study of Time Evolution of Thermal and Nonthermal Emission from an M-class Solar Flare
Achievements and Lessons Learned From Successful Small Satellite Missions for Space Weather-Oriented Research
Scaling of Electron Heating by Magnetization During Reconnection and Applications to Dipolarization Fronts and Super-Hot Solar Flares
Defining the Middle Corona
First Results for Solar Soft X-Ray Irradiance Measurements from the Third-generation Miniature X-Ray Solar Spectrometer
Deciphering the solar coronal heating: Energizing small-scale loops through surface convection
Using Potential Field Extrapolations to Explore the Origin of Type II Spicules
Phase mixed Alfvén waves in partially ionised solar plasmas
Terrestrial temperature, sea levels and ice area links with solar activity and solar orbital motion
A model of failed solar eruption initiated and destructed by magnetic reconnection
Energetics of a solar flare and a coronal mass ejection generated by a hot channel eruption

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