Diagnosing MHD Wave Detections in Solar Coronal Loops: Torsional Effects

Details Diagnosing MHD Wave Detections in Solar Coronal Loops: Torsional Effects Diagnosing MHD Wave Detections in Solar Coronal Loops: Torsional Effects

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.547..513w&link_type=abstract

Proceedings of 'SOHO 13 - Waves, Oscillations and Small-Scale Transient Events in the Solar Atmosphere: A Joint View from SOHO a

Computer Science

6

Sun, Waves, Corona, Mhd

Scientific paper

Filtergram instruments, such as TRACE, SoHO's EIT and the Solar Eclipse Corona Imaging System (SECIS) [1] have successfully detected MHD modes in coronal structures. However, all such experiments have suffered to varying degrees from the lack of (line-of-sight) velocity information. Trapped modes - torsional Alfvén waves, fast and slow kink and sausage waves - will all ideally manifest different velocity and density perturbation profiles, but current instrumentation cannot meet the spatial, spectral and temporal resolutions required to differentiate between these modes at high frequencies. Following work on optically thin line-of-sight effects in incompressible and compressible MHD wave modes, a model is presented of the observable spectral effects of a torsional wave passing through a loop.

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