E-Print Archive

There are 4618 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Exploring the Origin of Solar Energetic Electrons I: Constraining the Properties of the Acceleration Region Plasma Environment View all abstracts by submitter

Ross Pallister   Submitted: 2023-10-10 04:18

Solar flare electron acceleration is an efficient process, but its properties (mechanism, location) are not well constrained. Via hard X-ray (HXR) emission, we routinely observe energetic electrons at the Sun, and sometimes we detect energetic electrons in interplanetary space. We examine if the plasma properties of an acceleration region (size, temperature, density) can be constrained from in-situ observations, helping to locate the acceleration region in the corona, and infer the relationship between electrons observed in-situ and at the Sun. We model the transport of energetic electrons, accounting for collisional and non-collisional effects, from the corona into the heliosphere (to 1.0 AU). In the corona, electrons are transported through a hot, over-dense region. We test if the properties of this region can be extracted from electron spectra (fluence and peak flux) at different heliospheric locations. We find that cold, dense coronal regions significantly reduce the energy at which we see the peak flux and fluence for distributions measured out to 1.0 AU, the degree of which correlates with the temperature and density of plasma in the region. Where instrument energy resolution is insufficient to differentiate the corresponding peak values, the spectral ratio of [7-10) to [4-7) keV can be more readily identified and demonstrates the same relationship. If flare electrons detected in-situ are produced in, and/or transported through hot, over-dense regions close to HXR-emitting electrons, then this plasma signature should be present in their lower-energy spectra (1-20 keV), observable at varying heliospheric distances with missions such as Solar Orbiter.

Authors: Ross Pallister, Natasha L. S. Jeffrey
Projects: None

Publication Status: Accepted for publication in The Astrophysical Journal
Last Modified: 2023-10-10 11:01
Go to main E-Print page  Extreme Red-wing Enhancements of UV Lines During the 2022 March 30 X1.3 Solar Flare  APO & SMARTS flare star campaign observations I. Blue wing asymmetries in chromospheric lines during mid M dwarf flares from simultaneous spectroscopic and photometric observation data  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
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
An Optically Thin View of the Flaring Chromosphere: Nonthermal widths in a chromospheric condensation during an X-class solar flare
A Database of Magnetic and Thermodynamic Properties of Confined And Eruptive Solar Flares

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