Correlated Intensity Oscillations in the Upper Chromosphere and Upper Transition Region above Active Region Plage

Details Correlated Intensity Oscillations in the Upper Chromosphere and Upper Transition Region above Active Region Plage Correlated Intensity Oscillations in the Upper Chromosphere and Upper Transition Region above Active Region Plage

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.547...25d&link_type=abstract

Proceedings of 'SOHO 13 - Waves, Oscillations and Small-Scale Transient Events in the Solar Atmosphere: A Joint View from SOHO a

Computer Science

3

Magnetic Fields, Sun: Photosphere, Sun: Chromosphere, Sun: Transition, Sun: Corona

Scientific paper

Although there are now many observations showing the presence of oscillations in the corona, their direct relationship to waves or oscillations in the photosphere and chromosphere is not well understood. We provide an overview of recent studies describing correlations between oscillations in the lower and upper atmosphere. We focus in particular on our recent wavelet analysis of observations (made with TRACE, the Transition Region and Coronal Explorer) of strong ( 5 - 15%) intensity oscillations in the upper TR footpoints of hot coronal loops. They show a range of periods from 200 to 600 seconds, typically persisting for 4 to 7 cycles. These oscillations are not associated with sunspots, as they usually occur at the periphery of plage regions. A preliminary comparison to photospheric vertical velocities (using the Michelson Doppler Imager onboard SOHO) reveals that some upper TR oscillations show a correlation with p-modes in the photosphere. In addition, a majority of the upper TR oscillations are directly associated with upper chromospheric oscillations observed in H, i.e., periodic flows in spicular structures. The presence of such strong oscillations at low heights (of order 3,000 km) provides an ideal opportunity to study the propagation of oscillations from photosphere and chromosphere into the TR and corona. It can also help us understand the magnetic connectivity in the chromosphere and TR, and shed light on the source of chromospheric mass flows such as spicules.

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