Euv Imaging Of Shock Formation In The Low Corona With Sdo/aia

Details Euv Imaging Of Shock Formation In The Low Corona With Sdo/aia Euv Imaging Of Shock Formation In The Low Corona With Sdo/aia

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.0907v&link_type=abstract

American Astronomical Society, SPD meeting #42, #9.07; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Shock generation in the low corona has long been inferred by spectral observations of drifting so-called type-II radio emission in the metric wavelengths. Type-IIs occur with coronal mass ejections (CMEs) and/or flares but not consistently. Therefore, the exact relationship has been difficult to pin down, mostly because of the lack of radio imaging capability and of the low cadence of EUV observations in the low corona during the flare/CME formation. The advent of ultra-high observations from the AIA imagers has changed all that. In this talk, we present several direct observations of shock formation in the EUV and their association to the accompanying type-IIs. We will show that the coronal expansion driven by the formation of the CME ejecta is responsible for both EUV and radio emissions.

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