Interplanetary Type II Intensity Emission as a Function of the Heliospheric Position and Coronal Mass Ejection Speed

Details Interplanetary Type II Intensity Emission as a Function of the Heliospheric Position and Coronal Mass Ejection Speed Interplanetary Type II Intensity Emission as a Function of the Heliospheric Position and Coronal Mass Ejection Speed

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh51a1464a&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH51A-1464

Physics

7513 Coronal Mass Ejections (2101), 7534 Radio Emissions, 7847 Radiation Processes, 7851 Shock Waves (4455)

Scientific paper

Interplanetary Type II radio burst radiation results from the excitation of plasma waves in the ambient medium by a coronal mass ejection (CME) driven shock, propagating outward from the Sun. However, not all disturbances are able to produce Type II emission. Factors such as the speed of the disturbance and the properties of the medium through which the disturbance propagates are fundamental to produce Type II emission. Shock formation requires that the velocity of the disturbance excedes the local fast magnetosonic speed. Some studies have evaluated the radial behaviour of the fast magnetosonic speed as well as the Alfven speed above active regions. By combining both white light (SOHO/LASCO) and radio (Wind/WAVES) observations, we present preliminary results on the Type II intensity emission as a function of heliospheric position and CME speed. This might reveal the average Alfven speed profile in the inner heliosphere which, in turn, would tell us about the location of the solar wind acceleration. This work is supported by the University of California Institute for Mexico and the United States (UC MEXUS).

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