E-Print Archive

There are 4438 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Rayleigh-Taylor instabilities with sheared magnetic fields View all abstracts by submitter

Jaume Terradas   Submitted: 2014-02-27 05:16

Magnetic Rayleigh-Taylor (MRT) instabilities may play a relevant role in many astrophysical problems. In this work the effect of magnetic shear on the growth rate of the MRT instability is investigated. The eigenmodes of an interface and a slab model under the presence of gravity are analytically calculated assuming that the orientation of the magnetic field changes in the equilibrium, i.e., there is magnetic shear. We solve the linearised magnetohydrodynamic (MHD) equations in the incompressible regime.We find that the growth rate is bounded under the presence of magnetic shear. We have derived simple analytical expressions for the maximum growth rate, corresponding to the most unstable mode of the system. These expressions provide the explicit dependence of the growth rate on the various equilibrium parameters. For small angles the growth time is linearly proportional to the shear angle, and in this regime the single interface problem and the slab problem tend to the same result. On the contrary, in the limit of large angles and for the interface problem the growth time is essentially independent of the shear angle. In this regime we have also been able to calculate an approximate expression for the growth time for the slab configuration. Magnetic shear can have a strong effect on the growth rates of the instability. As an application of the results found in this paper we have indirectly determined the shear angle in solar prominence threads using their lifetimes and the estimation of the Alfvén speed of the structure.

Authors: Ruderman, M. S., Terradas, J., Ballester, J. L.
Projects: None

Publication Status: accpeted for publication in ApJ
Last Modified: 2014-02-27 13:37
Go to main E-Print page  Asymmetry in the CME-CME interaction process for the events from 2011 February 14-15  Solar Energetic Particle Events in the 23rd Solar Cycle: Interplanetary Magnetic Field Configuration and Statistical Relationship with Flares and CMEs  Edit Entry  Download Preprint  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
Variations of the Internal Asymmetries of Sunspot Groups During their Decay
Partial Eruption, Confinement, and Twist Buildup and Release of a Double-decker Filament
Overdense Threads in the Solar Corona Induced by Torsional Alfvén Waves
Implications of spicule activity on coronal loop heating and catastrophic cooling
The Magnetic Origin of Solar Campfires
On the evolution of a sub-C class flare: a showcase for the capabilities of the revamped Catania Solar Telescope
Direct evidence that twisted flux tube emergence creates solar active regions
Numerical Simulation of a Fundamental Mechanism of Solar Eruption with Different Magnetic Flux Distributions
Toward Improved Understanding of Magnetic Fields Participating in Solar Flares: Statistical Analysis of Magnetic Field within Flare Ribbons
Torus-Stable Zone Above Starspots
Constraining the CME Core Heating and Energy Budget with SOHO/UVCS
The solar corona as an active medium for magnetoacoustic waves
Rapid Evolution of Bald Patches in a Major Solar Eruption
Evaluating Pointing Strategies for Future Solar Flare Missions
Common origin of quasi-periodic pulsations in microwave and decimetric solar radio bursts
Thomson scattering in the lower corona in the presence of sunspots
The Spatial and Temporal Variations of Turbulence in a Solar Flare
Investigations of Sizes and Dynamical Motions of Solar Photospheric Granules by a Novel Granular Segmenting Algorithm
Millennial oscillations of solar irradiance and magnetic field at Earth in 600-2600
Plasma turbulence generated in 3D current sheet with magnetic islands

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