E-Print Archive

There are 4236 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.

Particle acceleration and transport during 3D CME eruptions View all abstracts by submitter

Valentina Zharkova   Submitted: 2020-04-26 03:23

We calculate particle acceleration during corona mass ejection (CME) eruptions using combined magnetohydrody- namic (MHD) and test-particle models. The 2.5D/3D CMEs are generated via the breakout mechanism. In this scenario a reconnection at the “breakout” current sheet (CS) above the flux rope initiates the CME eruption by destabilizing a quasi-static force balance. Reconnection at the flare CS below the erupting flux rope drives the fast acceleration of the CME, which forms flare loops below and produces the energetic particles observed in flares. For test-particle simulations, two times are selected during the impulsive and decay phases of the eruption. Particles are revealed to be accelerated more efficiently in the flare CS rather than in the breakout CS even in the presence of large magnetic islands. Particles are first accelerated in the CSs (with or without magnetic islands) by the reconnection electric field mainly through particle curvature drift. We find, as expected, that accelerated particles precipitate into the chromosphere, or become trapped in the loop top by magnetic mirrors, or escape to interplanetary space along open field lines. Some trapped particles are reaccelerated, either via reinjection to the flare CS or through a local Betatron-type acceleration associated with compression of the magnetic field. The energetic particles produce rela- tively hard energy spectra during the impulsive phase. During the gradual phase, the relaxation of magnetic field shear reduces the guiding field in the flare CS, which leads to a decrease in particle energization efficiency. Important implications of our results for observations of particle acceleration in the solar coronal jets are also discussed.

Authors: Qian Xia, Joel Dahlin, Valentina Zharkova and Spiro Antiochos
Projects: None

Publication Status: Astrophysica Journal, in press
Last Modified: 2020-04-27 10:45
Go to main E-Print page  Statistical Study of GOES X-ray Quasi-Periodic Pulsations in Solar   Flares  First Observation of a Type II Solar Radio Burst Transitioning between a Stationary and Drifting State  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
Sunquake with a second-bounce, other sunquakes and emission associated with X9.3 flare of 6 September 2017. II. Proposed interpretation
f-mode strengthening from a localized bipolar subsurface magnetic field
Imaging and spectral study on the null point of a fan-spine structure during a solar flare
Forecasting Solar Cycle 25 Using Deep Neural Networks
An Observational Test of Solar Plasma Heating by Magnetic Flux Cancellation
The Drivers of Active Region Outflows into the Slow Solar Wind
HXR emission from an activated flux rope and subsequent evolution of an eruptive long duration solar flare
A Survey of Computational Tools in Solar Physics
Sunquake with a second bounce, other sunquakes, and emission associated with the X9.3 flare of 6 September 2017. I. Observations
The PDFI_SS Electric Field Inversion Software
Spatial Distribution of Origin of Umbral Waves in a Sunspot Umbra
A Unique Resource for Solar Flare Diagnostic Studies: the SMM Bent Crystal Spectrometer
Inferring Vector Magnetic Fields from Stokes Profiles of GST/NIRIS Using a Convolutional Neural Network
Global Energetics of Solar Flares, X. Petschek Reconnection Rate and Alfvén Mach Number of Magnetic Reconnection Outflows
Transverse coronal loop oscillations excited by homologous circular-ribbon flares
Temporal evolution of oscillating coronal loops
Intrusion of Magnetic Peninsula toward the Neighboring Opposite-polarity Region That Triggers the Largest Solar Flare in Solar Cycle 24
On the Relationship Between Transit Time of ICMEs and Strength of the Initiated Geomagnetic Storms
Standing kink waves in sigmoid solar coronal loops: implications for coronal seismology
Excitation of negative energy surface magnetohydrodynamic waves in an incompressible cylindrical plasma

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