Photospheric Oscillations in the Solar Atmosphere: Driving Chromospheric Spicules and Coronal Waves

Details Photospheric Oscillations in the Solar Atmosphere: Driving Chromospheric Spicules and Coronal Waves Photospheric Oscillations in the Solar Atmosphere: Driving Chromospheric Spicules and Coronal Waves

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh13a1142d&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH13A-1142

Physics

7507 Chromosphere, 7509 Corona, 7524 Magnetic Fields, 7529 Photosphere, 7546 Transition Region

Scientific paper

There are now many observations of oscillations and waves with periods around 5 minutes in the solar transition region and corona. We provide an observational overview of 5 minute periodicity in upper transition region moss, the low legs of coronal loops, and chromospheric spicules in active region plage. The source of the 5 minute periodicity is unclear, since photospheric p-modes are evanescent in the upper photosphere which should prevent them from propagating into the chromosphere, transition region and corona. Using a numerical model we show that photospheric oscillations can propagate into the low atmosphere as long as they are guided along a magnetic flux tube that is inclined away from the vertical. The leaked photospheric oscillations develop non-linearly into shocks at low chromospheric heights because of the density decrease with height. The upward traveling shocks and resulting rebound shocks of the chromosphere lead to periodic upward chromospheric flows, which in a recent paper we have identified as the periodic spicules that we observe in active region plage. After passage through the spicule, these shocked photospheric oscillations propagate into the corona. We suggest that TRACE observations of propagating acoustic waves in the corona are shocked and tunneled photospheric oscillations. We also explore whether these coronal waves can be exploited to determine the connectivity between photosphere and corona, and thus perform seismology of the lower solar atmosphere.

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