Other
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh53b..03o&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #SH53B-03
Other
7599 General Or Miscellaneous, 7851 Shock Waves, 7863 Turbulence, 7899 General Or Miscellaneous
Scientific paper
The solar wind is a turbulent plasma in which shocks, waves, and discontinuities are observed to propagate away from the sun. Comparing data from several spacecraft in different places can yield information about the nature of these disturbances and their development. Among others, the present authors have studied correlations between Wind and SOHO plasma data for the period 1996 to 1999. In this paper we extend this work to cover the maximum of solar cycle 23 in the years 2001 and 2002. The observations are spaced 96 seconds apart and are correlated over 2-hour periods. We confirm a dependence of the mean value of the correlation coefficient upon solar activity, decreasing from 0.54 in 1996 to 0.47 in 2000. Using a list of shocks observed during the period 2000 and 2001, we find their directions of propagation to be distributed about the radial direction in a cone with a half angle of about 20 degrees, and a tendency for discontinuities to occur at angles grouped about the Parker spiral direction, as also earlier demonstrated by Coplan et al. and by the MIT group. In order to emphasize short time scale disturbances the data have been prewhitened. Correlations of these prewhitened data provide additional information about the evolution of solar wind stuuctures.
Coplan Michael A.
Ogilvie Keith. W.
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