E-Print Archive

There are 4414 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
Investigation on the Spatiotemporal Structures of Supra-Arcade Spikes View all abstracts by submitter

Rui Liu   Submitted: 2021-06-21 19:52

The vertical current sheet (VCS) trailing coronal mass ejections (CMEs) is the key place where the flare energy release and the CME buildup take place through magnetic reconnection. It is often studied from the edge-on perspective for the morphological similarity with the two-dimensional ``standard'' picture, but its three dimensional structure can only be revealed when the flare arcade is observed side on. The structure and dynamics in the so-called supra-arcade region thus contain important clues to the physical processes in flares and CMEs. Here we focus on the supra-arcade spikes (SASs), interpreted as the VCS viewed side-on, to study their spatiotemporal structures. By identifying each individual spike during the decay phase of four selected flares, in which the associated CME is traversed by a near-Earth spacecraft, we found that the widths of spikes are log-normal distributed, while the Fourier power spectra of the overall supra-arcade EUV emission, including bright spikes and dark downflows as well as the diffuse background, are power-law distributed, in terms of either spatial frequency k or temporal frequency ν, which reflects the fragmentation of the VCS. We demonstrate that coronal emission-line intensity observations dominated by Kolmogorov turbulence would exhibit a power spectrum of E(k)~k-13/3 or E(ν)~ ν-7/2, which is consistent with our observations. By comparing the number of SASs and the turns of field lines as derived from the ICMEs, we found a consistent axial length of ~3.5 AU for three events with a CME speed of ~1000 km s-1 in the inner heliosphere, but a much longer axial length ~8 AU) for the fourth event with an exceptionally fast CME speed of ~1500 km s-1, suggesting that this ICME is flattened and its `nose' has well passed the Earth when the spacecraft traversed its leg.

Authors: Rui Liu & Yuming Wang
Projects: None

Publication Status: accepted for publication in A&A
Last Modified: 2021-06-23 03:08
Go to main E-Print page  Validation of the PDFI_SS method for electric field inversions using a magnetic flux emergence simulation  Magnetic helicity and energy budget around large confined and eruptive solar flares  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
Formation of Magnetic Flux Rope during Solar Eruption. I. Evolution of Toroidal Flux and Reconnection Flux
Stereoscopy of extreme UV quiet Sun brightenings observed by Solar Orbiter/EUI
Solar Flare Effects on the Earth’s Lower Ionosphere
Measurements of Photospheric and Chromospheric Magnetic Field Structures Associated with Chromospheric Heating over a Solar Plage Region
Probing Current Sheet Instabilities from Flare Ribbon Dynamics
Global Nature of Solar Coronal Shock Waves shown by Inconsistency between EUV Waves and Type II Radio Bursts
Solar surges related to UV bursts: Characterization through k-means, inversions and density diagnostics
A revised cone model and its application to non-radial prominence eruptions
Zonal harmonics of solar magnetic field for solar cycle forecast
TESS observations of flares and quasi-periodic pulsations from low mass stars and potential impact on exoplanets
Kink oscillations of coronal loops
First Frequency-Time-Resolved Imaging Spectroscopy Observations of Solar Radio Spikes
Magnetic Flux and Magnetic Non-potentiality of Active Regions in Eruptive and Confined Solar Flares
Observations of shock propagation through turbulent plasma in the solar corona
The Formation and Lifetime of Outflows in a Solar Active Region
Localised acceleration of energetic particles by a weak shock in the solar corona
Stereoscopic Measurements of Coronal Doppler Velocities
Multi-wavelength Observations of a Metric Type-II Event
A physics-based method that can predict imminent large solar flares
The Solar Memory From Hours to Decades

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