Alfven Waves in the Solar Corona

Details Alfven Waves in the Solar Corona Alfven Waves in the Solar Corona

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh21a0289t&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH21A-0289

Physics

7509 Corona, 7594 Instruments And Techniques, 7836 Mhd Waves And Instabilities (2149, 2752, 6050)

Scientific paper

We present observations of the coronal intensity, line-of-sight velocity, and linear polarization obtained in the FeXIII 1074.7 nm coronal emission line with the Coronal Multi-channel Polarimeter (CoMP) instrument. Analysis of these observations reveal ubiquitous upward propagating waves with phase speeds of 1-4 Mm/s and trajectories consistent with the direction of the magnetic field inferred from the linear polarization measurements. We can definitively identify these as Alfvén waves. An estimate of the energy carried by the waves that we spatially resolve indicates that they are unable to heat the solar corona, however, unresolved waves may carry sufficient energy.

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