Heliospheric remote imaging and its relation to CME input to solar wind propagation models

Details Heliospheric remote imaging and its relation to CME input to solar wind propagation models Heliospheric remote imaging and its relation to CME input to solar wind propagation models

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh24a..04p&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH24A-04

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7924] Space Weather / Forecasting, [7959] Space Weather / Models

Scientific paper

The process of transitioning the WSA-Enlil solar wind forecast model into operations at the National Weather Service provides an opportunity to reconsider the nature of CME inputs as determined from coronagraph and heliospheric imaging observations. At present, the model uses an extremely simple hydrodynamic pulse (increase in density and speed over the inferred angular extent of the CME) to mimic the driver gas at the base of the interplanetary (IP) regime. However, it is clear from recent events (as well as from analyses of STEREO/LASCO events by others) that the form of the CME in the corona is in many cases quite complex, such that it is unclear what input to provide to this model or any IP model. It appears that fast CMEs in particular consist - in the corona - of a visible mass driver (with significant magnetic structure) surrounded by a strong, spreading wavefront. What is important for forecasting is to understand what part of that full structure actually contributes to the IP propagation, and what part dissipates near the near Sun. A serious study of the propagation of strong shocks in a structured corona and out into the hyperalvenic regime is one element needed to improve modeling capabilities; another would be to tie the coronal observations to more distant heliospheric imagery for a collection of such events.

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