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Inversion of physical parameters in solar atmospheric seismology View all abstracts by submitter

Inigo Arregui   Submitted: 2012-03-14 04:38

Magnetohydrodynamic (MHD) wave activity is ubiquitous in the solar atmosphere. MHD seismology aims to determine difficult to measure physical parameters in solar atmospheric magnetic and plasma structures by a combination of observed and theoretical properties of MHD waves and oscillations. This technique, similar to seismology or helio-seismology, demands the solution of two problems. The direct problem involves the computation of wave properties of given theoretical models. The inverse problem implies the calculation of unknown physical parameters, by means of a comparison of observed and theoretical wave properties. Solar atmospheric seismology has been successfully applied to different structures such as coronal loops, prominence fine structures, spicules, or jets. However, it is still in its infancy. Far more is there to come. We present an overview of recent results, with particular emphasis on the inversion procedure.

Authors: I. Arregui
Projects: None

Publication Status: Review paper to appear in Astrophysics and Space Science Proceedings
Last Modified: 2012-03-14 14:08
Go to main E-Print page  Morphological evolution of a 3D CME cloud reconstructed from three viewpoints  A multiwavelength study of an M-class flare and the origin of an associated eruption from NOAA AR 11045  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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