Solar wind structure suggested by bimodal correlations of solar wind speed and density between the spacecraft SOHO and Wind

Details Solar wind structure suggested by bimodal correlations of solar wind speed and density between the spacecraft SOHO and Wind Solar wind structure suggested by bimodal correlations of solar wind speed and density between the spacecraft SOHO and Wind

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgra..11208104o&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue A8, CiteID A08104

Physics

1

Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Solar Wind Sources, Interplanetary Physics: Discontinuities (7811), Interplanetary Physics: Interplanetary Shocks

Scientific paper

We calculate the cross-spacecraft maximum lagged-cross-correlation coefficients for 2-hour intervals of solar wind speed and density measurements made by the plasma instruments on the Solar and Heliospheric Observatory (SOHO) and Wind spacecraft over the period from 1996, the minimum of solar cycle 23, through the end of 2005. During this period, SOHO was located at L1, about 200 R E upstream from the Earth, while Wind spent most of the time in the interplanetary medium at distances of more than 100 R E from the Earth. Yearly histograms of the maximum, time-lagged correlation coefficients for both the speed and density are bimodal in shape, suggesting the existence of two distinct solar wind regimes. The larger correlation coefficients we suggest are due to structured solar wind, including discontinuities and shocks, while the smaller are likely due to Alfvénic turbulence. While further work will be required to firmly establish the physical nature of the two populations, the results of the analysis are consistent with a solar wind that consists of turbulence from quiet regions of the Sun interspersed with highly filamentary structures largely convected from regions in the inner solar corona. The bimodal appearance of the distributions is less evident in the solar wind speed than in the density correlations, consistent with the observation that the filamentary structures are convected with nearly constant speed by the time they reach 1 AU. We also find that at solar minimum the fits for the density correlations have smaller high-correlation components than at solar maximum. We interpret this as due to the presence of more relatively uniform Alfvénic regions at solar minimum than at solar maximum.

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