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CME Propagation Characteristics from Radio Observations View all abstracts by submitter

Silja Pohjolainen   Submitted: 2007-07-11 10:47

We explore the relationship among three coronal mass ejections (CMEs), observed on 28 October 2003, 7 November 2004, and 20 January 2005, the type II burst-associated shock waves in the corona and solar wind, as well as the arrival of their related shock waves and magnetic clouds at 1 AU. Using six different coronal/interplanetary density models, we calculate the speeds of shocks from the frequency drifts observed in metric and decametric radio wave data. We compare these speeds with the velocity of the CMEs as observed in the plane-of-the-sky white-light observations and calculated with a cone model for the 7 November 2004 event. We then follow the propagation of the ejecta using Interplanetary Scintillation (IPS) measurements, which were available for the 7 November 2004 and 20 January 2005 events. Finally, we calculate the travel time of the interplanetary (IP) shocks between the Sun and Earth and discuss the velocities obtained from the different data. This study highlights the difficulties in making velocity estimates that cover the full CME propagation time.

Authors: S. Pohjolainen, L. van Driel-Gesztelyi, J.L. Culhane, P.K. Manoharan, H.A. Elliott
Projects: None

Publication Status: Solar Physics Topical Issue (Sun-Earth Connection), accepted July 2007
Last Modified: 2007-07-11 12:10
Go to main E-Print page  From GHz to mHz: A Multiwavelength Study of the Acoustically Active August 2004 M7.4 Solar Flare  The unpredictability of the most energetic solar events  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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