E-Print Archive

There are 3758 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
Optimal Energy Growth in Current Sheets View all abstracts by submitter

David MacTaggart   Submitted: 2017-09-14 08:21

In this paper, we investigate the possibility of transient growth in the linear perturbation of current sheets. The resistive magnetohydrodynamic (MHD) operator for a background field consisting of a current sheet is non-normal, meaning that associated eigenvalues and eigenmodes can be very sensitive to perturbation. In a linear stability analysis of a tearing current sheet, we show that modes that are damped as t\rightarrow\infty can produce transient energy growth, contributing faster growth rates and higher energy attainment (within a fixed finite time) than the unstable tearing mode found from normal-mode analysis. We determine the transient growth for tearing-stable and tearing-unstable regimes and discuss the consequences of our results for processes in the solar atmosphere, such as flares and coronal heating. Our results have significant potential impact on how fast current sheets can be disrupted. In particular, transient energy growth due to (asymptotically) damped modes may lead to accelerated current sheet thinning and, hence, a faster onset of the plasmoid instability, compared to the rate determined by the tearing mode alone.

Authors: David MacTaggart, Peter Stewart
Projects: None

Publication Status: Accepted for Solar Physics
Last Modified: 2017-09-15 10:13
Go to main E-Print page  The 17 February 2013 sunquake in the context of the active region's magnetic field configuration  Long- and Mid-Term Variations of the Soft X-ray Flare Type in Solar Cycles  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
Reconstruction of a Large-scale Pre-flare Coronal Current Sheet Associated with an Homologous X-shaped Flare
Comparison of Two Coronal Magnetic Field Models for Reconstructing a Sigmoidal Solar Active Region With Coronal Loops
A Magnetic Bald-Patch Flare in Solar Active Region 11117
Reply to comment by Usoskin (2017) on the paper
Non-thermal hydrogen Balmer and Paschen emission in solar flares generated by electron beams
Pulsations in the Earth's Lower Ionosphere Synchronized with Solar Flare Emission
Oscillations Excited by Plasmoids Formed During Magnetic Reconnection in a Vertical Gravitationally Stratified Current Sheet
Doppler shift oscillations from a hot line observed by IRIS
Dispersive Evolution of Nonlinear Fast Magnetoacoustic Wave Trains
Detection of 3-Minute Oscillations in Full-disk Lya Emission During A Solar Flare
A Compressed Sensing-based Image Reconstruction Algorithm for Solar Flare X-Ray Observations
Comparison of Helioseismic Far-side Active Region Detections with STEREO Far-Side EUV Observations of Solar Activity
Observations of a Radio-quiet Solar Preflare
Energy release in the solar atmosphere from a stream of infalling prominence debris
Estimation of a Coronal Mass Ejection Magnetic Field Strength using Radio Observations of Gyrosynchrotron Radiation
QUASI-PERIODIC OSCILLATIONS IN FLARES AND CORONAL MASS EJECTIONS ASSOCIATED WITH MAGNETIC RECONNECTION
The 17 February 2013 sunquake in the context of the active region's magnetic field configuration
Optimal Energy Growth in Current Sheets
Long- and Mid-Term Variations of the Soft X-ray Flare Type in Solar Cycles
The Abundance of Helium in the Source Plasma of Solar Energetic Particles

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