E-Print Archive

There are 4293 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
* 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.

The behavior of transverse waves in nonuniform solar flux tubes. I. Comparison of ideal and resistive results View all abstracts by submitter

Roberto Soler   Submitted: 2013-09-16 09:07

Magnetohydrodynamic (MHD) waves are ubiquitously observed in the solar atmosphere. Kink waves are a type of transverse MHD waves in magnetic flux tubes that are damped due to resonant absorption. The theoretical study of kink MHD waves in solar flux tubes is usually based on the simplification that the transverse variation of density is confined to a nonuniform layer much thinner than the radius of the tube, i.e., the so-called thin boundary approximation. Here, we develop a general analytic method to compute the dispersion relation and the eigenfunctions of ideal MHD waves in pressureless flux tubes with transversely nonuniform layers of arbitrary thickness. Results for kink waves are produced and are compared with fully numerical resistive MHD eigenvalue computations in the limit of small resistivity. We find that the frequency and resonant damping rate are the same in both ideal and resistive cases. The actual results for thick nonuniform layers deviate from the behavior predicted in the thin boundary approximation and strongly depend on the shape of the nonuniform layer. The eigenfunctions in ideal MHD are very different from those in resistive MHD. The ideal eigenfunctions display a global character regardless of the thickness of the nonuniform layer, while the resistive eigenfunctions are localized around the resonance and are indistinguishable from those of ordinary resistive Alfvén modes. Consequently, the spatial distribution of wave energy in the ideal and resistive cases is dramatically different. This poses a fundamental theoretical problem with clear observational consequences.

Authors: R. Soler, M. Goossens, J. Terradas, R. Oliver
Projects: None

Publication Status: Accepted for publication in ApJ
Last Modified: 2013-09-16 11:32
Go to main E-Print page   Twisting solar coronal jet launched at the boundary of an active region   Kinetic Alfv?n Turbulence and Parallel Electric Fields in Flare Loops  Edit Entry  Download Preprint  Submitter's Homepage 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
Non-Neutralized Electric Current of Active Regions Explained as a Projection Effect
The effect of magnetic field on the damping of slow waves in the solar corona
Soft X-Ray Observations of Quiescent Solar Active Regions using Novel Dual-zone Aperture X-ray Solar Spectrometer (DAXSS)
Proper Orthogonal and Dynamic Mode Decomposition of Sunspot Data.
Statistical Properties of Superflares on Solar-type Stars: Results Using All of the Kepler Primary Mission Data
Turbulent viscosity and effective magnetic Prandtl number from simulations of isotropically forced turbulence
Time and Charge-Sign Dependence of the Heliospheric Modulation of Cosmic Rays
Bayesian Analysis of Quasi-periodic Pulsations in Stellar Flares
Cause and Kinematics of a Jetlike CME
The role of small-scale surface motions in the transfer of twist to a solar jet from a remote stable flux rope
Sub-second time evolution of Type III solar radio burst sources at fundamental and harmonic frequencies
Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare
Differential rotation of the solar corona: A new data-adaptive multiwavelength approach
Magnetic Helicity Flux across Solar Active Region Photospheres: I. Hemispheric Sign Preference in Solar Cycle 24
Seismological constraints on the solar coronal heating function
The Coronal Global Evolutionary Model: Using HMI Vector Magnetogram and Doppler Data to Determine Coronal Magnetic Field Evolution
Radio and X-ray Observations of Short-lived Episodes of Electron Acceleration in a Solar Microflare
Research progress based on observations of the New Vacuum Solar Telescope
Dynamics evolution of a solar active-region filament from quasi-static state to eruption: rolling motion, untwisting motion, material transfer, and chirality
Microwave Study of a Solar Circular Ribbon Flare

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