Detection of Waves in the Solar Corona: Kink or Alfvén?

Details Detection of Waves in the Solar Corona: Kink or Alfvén? Detection of Waves in the Solar Corona: Kink or Alfvén?

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.2.81v&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

Last year, Tomczyk et al. (2007) have conclusively proven that low amplitude (1km/s) waves are ubiquitously present in the corona. A few months later, this was followed up with the discovery that chromospheric spicules carry tremendous wave power (De Pontieu et al., 2007). These new developments form a basis for coronal seismological magnetic field mapping of the corona and chromosphere. However, this must be based upon a confident identification of the observed wave mode.
Using basic MHD wave theory, we demonstrate that the only way to interpret the observed wave motions is in terms of fast magnetoacoustic kink waves. We prove that the interpretation in terms of Alfven waves, as was put forward in the original articles, does not explain the observed phenomenology, while the fast magnetoacoustic kink waves reproduce the required observational constraints.
To underline the potential of magnetic field mapping, we discuss a recent observation of coronal loop kink oscillations observed with Hinode/EIS. Because of its spectroscopic and imaging capabilities, we are able to measure the loop density, simultaneously with the loop length. This allows us to determine the magnetic field with unprecedented accuracy.

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