Coronal Mass Ejections and Interplanetary Scintillation

Details Coronal Mass Ejections and Interplanetary Scintillation Coronal Mass Ejections and Interplanetary Scintillation

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..317v&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Computer Science

Scientific paper

Excellent set of observations of coronal mass ejections are now available from Yohkoh and SOHO. It has become possible to investigate the initial ejection and acceleration of these from the X-ray images. The monitoring of propagation of the coronal mass ejections away from the Sun in the heliosphere is only possible by an indirect method of interplanetary scintillation (IPS). This phenomenon is sensitive to the presence and propagation of plasma irregularities crossing the line of site to a compact radio source from the observing radio telescope. The passage of a coronal mass ejection through the heliosphere is usually termed as interplanetary disturbance (IPD). Here we present the case studies of few selected coronal mass ejections and their associated IPDs. One of these a halo CME with a bright front (as seen in SOHO/LASCO) began on April 04, 2000 at about 1632 UT. This was associated with C9 flare in AR 8933. The IPS observations at 103 MHz detected the effect of this CME two days later at the line of sight of 3C459 and three days later at the line of sight of 3C2, 3C119 and 3C122. At the line of sight of 3C48 there appeared a very feeble effect of this CME. The CME of April 4, 2000 produced a shock which was detected by ACE solar wind velocity measurement (the radial velocity increased from 375 km/sec to 575 km/sec at 16 UT on April 6, 2000). We will compare shock magnitude with acceleration measured by SOHO images of the CME. This shock led to a very large drop (about 300 NT) in equatorial Dst and produced one of the largest geomagnetic storm. Here we will discuss these events in complete detail from their origin at Sun up to their interaction with the terrestrial environment. We will also inter compare the terrestrial impact of these events observed by IPS.

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