Inversion of Physical Parameters in Solar Atmospheric Seismology

Conference paper
Part of the Astrophysics and Space Science Proceedings book series (ASSSP, volume 33)


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 plasmas, 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 in the inversion procedure.


Coronal Loop Density Contrast Magnetic Flux Tube Kink Mode Period Ratio 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.



The author acknowledges the financial support received from the Spanish MICINN and FEDER funds under Grant No. AYA2006-07637. The author is also grateful to the Solar Physics Group members at Universitat de les Illes Balears, for many years of fruitful work.


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© Springer-Verlag Berlin Heidelberg 2012

Authors and Affiliations

  1. 1.Departament de FísicaUniversitat de les Illes BalearsPalma de MallorcaSpain

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