E-Print Archive

There are 4053 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
The influence of the internal structuring of coronal loops on the properties of their damped transverse oscillations View all abstracts by submitter

Inigo Arregui   Submitted: 2007-02-08 07:37

The geometry and physical conditions in solar coronal loops are complicated and still not well understood. Recent high resolution observations, obtained with TRACE, indicate the existence of sub-resolution transverse structuring, not accessible to direct observation. This ingredient has not yet been taken into account in previous theoretical models used for the study of transversal coronal loop oscillations and their damping due to resonant conversion of energy. This study aims to assess the effect of the possibly unresolved internal structure of a coronal loop on the properties of its transverse oscillations and on the efficiency of resonant absorption as a damping mechanism of these oscillations. The equilibrium configuration of a single coronal loop with internal density structuring is modelled by considering the loop as being composed by two very close parallel identical coronal slabs in Cartesian geometry. The period of the oscillation and the damping time, for the resonantly damped fundamental kink mode, are computed. These quantities are then compared to those obtained for two models for a single equivalent slab without internal density structuring. We find that the period and the damping time of a coronal loop with internal density structuring change by less than 15%, when compared to the same oscillatory properties of a single coronal loop with either the same density contrast or a single coronal loop with the same total mass. Therefore the internal density structuring of a coronal loop does not affect very much its oscillatory properties. However, the sub-resolution structuring of a coronal loop, with different densities in its components or with different widths could vary these results.

Authors: I. Arregui, J. Terradas, R. Oliver, & J.L. Ballester
Projects:

Publication Status: A&A, Vol. 466, 1145-1151 (2007)
Last Modified: 2007-04-26 02:46
Go to main E-Print page  A NOTE ON SATURATION SEEN IN THE MDI/SOHO MAGNETOGRAMS  A new method of observing weak extended sources with RHESSI  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
Linear waves in a non-equilibrium ionisation partially ionised plasma
How Many Twists Do Solar Coronal Jets Release?
Different Signatures of Chromospheric Evaporation in Two Solar Flares Observed with IRIS
The Physical Nature of Spiral Wave Patterns in Sunspots
Predicting Solar Flares Using a Long Short-Term Memory Network
Coronal loop transverse oscillations excited by different driver frequencies
Solar Center-Limb Variation of the Strengths of Spectral Lines: Classification and Interpretation of Observed Trends
The plasmoid instability in a confined solar flare
High-frequency dynamics of active region moss as observed by IRIS
Extreme-ultraviolet Late Phase Caused by Magnetic Reconnection over Quadrupolar Magnetic Configuration in a Solar Flare
Two-step evolution of a rising flux rope resulting in a confined solar flare
Why torus-unstable solar filaments experience failed eruption?
The Magnetic Properties of Heating Events on High-Temperature Active Region Loops
Pulse-beam heating of deep atmospheric layers, their oscillations and shocks modulating the flare reconnection
A potential magnetic field calculator for solar physics applications using staggered grids
E and B polarizations from inhomogeneous and solar surface turbulence
Oscillations Accompanying a He I 10830 Å Negative Fare in a Solar Facula II. Response of the Transition Region and Corona
Flare reconnection-driven magnetic field and Lorentz force variations at the Sun's surface
Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?
Impacts On Proton Fluxes Observed During Different Interplanetary Conditions

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