Physics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh53a..08r&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SH53A-08
Physics
6964 Radio Wave Propagation, 7513 Coronal Mass Ejections, 7534 Radio Emissions
Scientific paper
There has been much discussion and debate about how CMEs propagate from the solar corona to Earth, including their interactions and the relationship of the driver to the shock. The coronal propagation of CMEs is fairly well determined out to 30 Rs from existing space-based and ground-based coronagraphs. At the present time there are four ways to obtain information on the interplanetary transport of CMEs: IPS and low-frequency radio observations (e.g., various ground-based radio telescopes and space-based Wind/WAVES), white-light all-sky images (SMEI), and a variety of gas-dynamic and MHD models. These various observations and models, all of which have advantages and disadvantages, often give very different results for the kinematics of interplanetary CMEs. The focus of discussion here is a simple quantitative model of the CME kinematics based on the constraints provided by the low-frequency radio observations and the calculated in-situ shock parameters, together with required consistency with the white-light measurements, to deduce the kinematics of interplanetary CMEs. This simple model seems to agree with the white-light SMEI observations in the one case where it has been tested. The above model has been applied to a number of CMEs for which there were good low-frequency radio observations (from Wind/WAVES) and well-defined shock signatures at 1 AU. The analyses of these events provide quantitative insights into how fast CMEs decelerate in the interplanetary medium. The validity of this model will be more directly tested using the STEREO observations. In addition to the white-light and radio observations that are presently available from various interplanetary spacecraft, the STEREO mission will enable some unique measurements such as radio source triangulation, which will provide additional constraints on the determination of CME propagation. These STEREO radio observations, together with the white-light observation from the Heliospheric Imager, may clarify the relationship of the shock to the CME driver during the interplanetary transport of CMEs.
Kaiser Michael L.
Reiner M. J.
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