Variability in the slow solar wind at solar minimum

Details Variability in the slow solar wind at solar minimum Variability in the slow solar wind at solar minimum

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh33c..04b&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH33C-04

Physics

[2102] Interplanetary Physics / Corotating Streams, [2162] Interplanetary Physics / Solar Cycle Variations, [2169] Interplanetary Physics / Solar Wind Sources

Scientific paper

Analysis at high time resolution of radio scintillation observations made using the EISCAT facility of the slow solar wind during late April and early May 2007 suggested the presence of a considerable degree of small- and medium-scale structure, characterised by intervals of rapid field rotation. This hypothesis was supported by the large number of medium-scale transient structures seen by the Heliospheric Imagers carried by the twin NASA STEREO spacecraft and by the continued activity of the comet P-Encke in the aftermath of its tail disconnection event. However, it was not apparent from this interval whether this degree of fine-scale structure was a normal feature of the solar minimum slow wind or whether it reflected the particular characteristics of the outflow in the aftermath of a mass ejection. In this paper we present the results of high time resolution analysis of radio scintillation observations of the slow wind from the last two solar minima and compare them with STEREO observations and in-situ measurements in the cases when these are available.

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