E-Print Archive

There are 4330 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.

Quasi-Periodic Particle Acceleration in a Solar Flare View all abstracts by submitter

Brendan Clarke   Submitted: 2021-02-10 14:23

A common feature of electromagnetic emission from solar flares is the presence of intensity pulsations that vary as a function of time. Known as quasi-periodic pulsations (QPPs), these variations in flux appear to include periodic components and characteristic time-scales. Here, we analyse a GOES M3.7 class flare exhibiting pronounced QPPs across a broad band of wavelengths using imaging and time-series analysis. We identify QPPs in the timeseries of X-ray, low frequency radio and EUV wavelengths using wavelet analysis, and localise the region of the flare site from which the QPPs originate via X-ray and EUV imaging. It was found that the pulsations within the 171 Ȧ, 1600 Ȧ, soft X-ray (SXR), and hard X-ray (HXR) light curves yielded similar periods of ∼122 s, ∼131s, ∼123 s, and ∼137 s, respectively, indicating a common progenitor. The low frequency radio emission at 2.5 MHz contained a longer period of ∼231 s. Imaging analysis indicates that the location of the X-ray and EUV pulsations originates from a HXR footpoint linked to a system of nearby open magnetic field lines. Our results suggest that intermittent particle acceleration, likely due to 'bursty' magnetic reconnection, is responsible for the QPPs. The precipitating electrons accelerated towards the chromosphere produce the X-ray and EUV pulsations, while the escaping electrons result in low frequency radio pulses in the form of type III radio bursts. The modulation of the reconnection process, resulting in episodic particle acceleration, explains the presence of these QPPs across the entire spatial range of flaring emission.

Authors: Brendan P. Clarke, Laura A. Hayes, Peter T. Gallagher, Shane A. Maloney, Eoin P. Carley
Projects: Fermi/GBM,GOES X-rays,RHESSI,SDO-AIA,SDO-HMI,Wind

Publication Status: Accepted
Last Modified: 2021-02-10 23:38
Go to main E-Print page   Transition to turbulence in nonuniform coronal loops driven by torsional Alfven waves   Relationship between three-dimensional velocity of filament eruptions and CME association  Edit Entry  Download Preprint  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
The effect of a dynamo-generated field on the Parker wind
Magnetic Helicity Flux across Solar Active Region Photospheres: II. Association of Hemispheric Sign Preference with Flaring Activity during Solar Cycle 24
NuSTAR Observation of Energy Release in 11 Solar Microflares
The Lyα Emission in Solar Flares. I. A Statistical Study on Its Relationship with the 1-8 Soft X-Ray Emission
Radiative hydrodynamic simulations of the spectral characteristics of solar white-light flares
Slow-Mode Magnetoacoustic Waves in Coronal Loops (Review)
Diagnosing a Solar Flaring Core with Bidirectional Quasi-periodic Fast Propagating Magnetoacoustic Waves
Are the brightest coronal loops always rooted in mixed-polarity magnetic flux?
Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections
Properties of stream interaction regions at Earth and Mars during the declining phase of SC 24
Spatial and temporal analysis of 3-minute oscillations in the chromosphere associated with the X2.2 Solar Flare on 2011 February 15
Pitch-angle distribution of accelerated electrons in 3D current sheets with magnetic islands
Transition to turbulence in nonuniform coronal loops driven by torsional Alfvén waves
Quasi-Periodic Particle Acceleration in a Solar Flare
Relationship between three-dimensional velocity of filament eruptions and CME association
Multi-thermal atmosphere of a mini-solar flare during magnetic reconnection observed with IRIS
Solar Irradiance Variability Due To Solar Flares Observed in Lyman α Emission
Evolutionary stages and triggering process of a complex eruptive flare with circular and parallel ribbons
Sequential Lid Removal in a Triple-decker Chain of CME-producing Solar Eruptions
The Neupert Effect of Flare UltraViolet and Soft X-ray Emissions

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