Latitudinal Extent of Large Scale Solar Wind Structures

Details Latitudinal Extent of Large Scale Solar Wind Structures Latitudinal Extent of Large Scale Solar Wind Structures

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh32a0730e&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH32A-0730

Physics

2102 Corotating Streams, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2164 Solar Wind Plasma

Scientific paper

In this study we examine solar wind observations from two spacecraft widely separated in helocentric latitude in order to determine the latitudinal exent of large scale solar wind structures. In particular, we compare solar wind plasma observations obtained from ACE near 1 AU to those of Ulysses between 2 and 5.5 AU from the start of 1998 through day 200 of year 2000. We account for solar wind evolution with distance by propagating the ACE measurements to the position of Ulysses using a single-fluid hydrodynamic code. We also shift the ACE measurements in time in order to compare parcels from the same source longitude. Based on the comparison of plasma parameters and magnetic sectors, we find that a number of the large scale structures can be readily identified over latitudinal separations of several tens of degrees. We quantify the coherence of coronal mass ejections and stream interaction regions as a function of latitudinal extent.

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