Solar p-mode frequency plasma waves in high speed solar wind streams

Details Solar p-mode frequency plasma waves in high speed solar wind streams Solar p-mode frequency plasma waves in high speed solar wind streams

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh21b1917b&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH21B-1917

Physics

Plasma Physics

[7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7800] Space Plasma Physics, [7900] Space Weather, [7954] Space Weather / Magnetic Storms

Scientific paper

We report our finding that discrete plasma wave frequencies in the 3-20 minute period band (solar p-mode frequencies) are concentrated in high speed solar wind streams originating from solar coronal holes. The results are based on analysis of solar wind proton velocities measured by the SWEPAM (Solar Wind Electron, Proton, and Alpha Monitor) instrument on board the ACE (Advanced Composition Explorer) satellite. The analysis spans several solar rotations (CIR events) during the quiet sun period of June through August 2008, when CME and other transient solar-produced events were absent. Waves in the solar wind plasma may carry signatures of the Sun's interior structure, and dynamics in the chromosphere and corona. This finding adds important new insights to past findings that solar p-mode frequencies propagate as plasma waves into the interplanetary medium. The dominance of such waves in the high speed streams implies that the open field lines from solar polar coronal holes provide a key path for the waves to propagate to large distances from the Sun.

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