Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11d..02b&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SH11D-02
Physics
2111 Ejecta, Driver Gases, And Magnetic Clouds, 7513 Coronal Mass Ejections
Scientific paper
There are at least two types of ejecta in the solar wind: magnetic clouds (in which the magnetic field direction rotates smoothly through a large angle) and complex ejecta (in which the magnetic field direction has a complex structure). Ejecta are generally associated with CMEs, but this association is not understood in detail. Near solar maximum, complex ejecta in the form of a single fast stream can be associated with a series of CMEs. Conversely, successive CMEs can interact and merge to form complex ejecta near 1 AU. More generally, a series of ejecta and corotating streams at 1 AU can form a transient flow system in which the individual streams interact and coalesce with increasing distance from the sun, forming larger structures. We shall show examples of the types of flows and flow systems mentioned above, including transient flow systems observed by Helios 1 during 1979, by ACE in May, 1998, and by ACE in July, 2000. Although these phenomena have been studied for many years, significant progress in understanding them is being made based on the recent nearly continuous in situ observations from WIND and ACE at 1 AU, the unprecedented composition observations from ACE, the high sensitivity coronagraph and EIT observations from SOHO, and realistic time-dependent 3-D MHD codes.
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