E-Print Archive

There are 3855 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Strong non-radial propagation of energetic electrons in solar corona View all abstracts by submitter

Andreas Klassen   Submitted: 2018-03-07 03:37

Analyzing the sequence of solar energetic electron events measured at both STEREO-A (STA) and STEREO-B (STB) spacecraft during 17-21 July 2014, when their orbital separation was 34?, we found evidence of a strong non-radial electron propagation in the solar corona below the solar wind source surface. The impulsive electron events were associated with recurrent flare and jet (hereafter flare/jet) activity at the border of an isolated coronal hole situated close to the solar equator. We have focused our study on the solar energetic particle (SEP) event on 17 July 2014, during which both spacecraft detected a similar impulsive and anisotropic energetic electron event suggesting optimal connection of both spacecraft to the parent particle source, despite the large angular separation between the parent flare and the nominal magnetic footpoints on the source surface of STA and STB of 68? and 90?, respectively. Combining the remote-sensing extreme ultraviolet (EUV) observations, in-situ plasma, magnetic field, and energetic particle data we investigated and discuss here the origin and the propagation trajectory of energetic electrons in the solar corona. We find that the energetic electrons in the energy range of 55-195 keV together with the associated EUV jet were injected from the flare site toward the spacecraft?s magnetic footpoints and propagate along a strongly non-radial and inclined magnetic field below the source surface. From stereoscopic (EUV) observations we estimated the inclination angle of the jet trajectory and the respective magnetic field of 63? ? 11? relative to the radial direction. We show how the flare accelerated electrons reach very distant longitudes in the heliosphere, when the spacecraft are nominally not connected to the particle source. This example illustrates how ballistic backmapping can occasionally fail to characterize the magnetic connectivity during SEP events. This finding also provides an additional mechanism (one among others), which may explain the origin of widespread SEP events.

Authors: A. Klassen, N. Dresing, R. Gómez-Herrero, B. Heber, and A. Veronig

Publication Status: Accepted in A&A
Last Modified: 2018-03-07 13:04
Go to main E-Print page  Forward Modeling of Coronal Mass Ejection Flux Ropes in the Inner Heliosphere with 3DCORE  Developments of Multi-wavelength Spectro-Polarimeter on the Domeless Solar Telescope at Hida Observatory  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
Propagation of a global coronal wave and its interaction with large-scale coronal magnetic structures
A New Tool for CME Arrival Time Prediction Using Machine Learning Algorithms: CAT-PUMA
Solar Magnetoseismology with Magnetoacoustic Surface Waves in Asymmetric Magnetic Slab Waveguides
Blue wing enhancement of the chromospheric Mg II h and k lines in a solar flare
Finite amplitude transverse oscillations of a magnetic rope
Bridging the Gap: Capturing the Lyα Counterpart of a Type-II Spicule and its Heating Evolution with VAULT2.0 and IRIS Observations
Turbulent transport coefficients in spherical wedge dynamo simulations of solar-like stars
Implosive collapse about magnetic null points: A quantitative comparison between 2D and 3D nulls
Forward Modeling of Coronal Mass Ejection Flux Ropes in the Inner Heliosphere with 3DCORE
Strong non-radial propagation of energetic electrons in solar corona
Developments of Multi-wavelength Spectro-Polarimeter on the Domeless Solar Telescope at Hida Observatory
LOFAR observations of the quiet solar corona
Statistics of "Cold" Early Impulsive Solar Flares in X-ray and Microwave domains
Successive X-class flares and coronal mass ejections driven by shearing motion and sunspot rotation in active region NOAA 12673
An Observationally-Constrained Model of a Flux Rope that Formed in the Solar Corona
The Duration of Energy Deposition on Unresolved Flaring Loops in the Solar Corona
On the detection of coronal dimmings and the extraction of their characteristic properties
Plasma diagnostics of coronal dimming events
Multi-fluid approach to high-frequency waves in plasmas. III. Nonlinear regime and plasma heating
Observationally quantified reconnection providing a viable mechanism for active region coronal heating

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