Interplanetary consequences caused by the extremely intense solar activity during October-November 2003

Details Interplanetary consequences caused by the extremely intense solar activity during October-November 2003 Interplanetary consequences caused by the extremely intense solar activity during October-November 2003

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jgra..11001109t&link_type=abstract

Journal of Geophysical Research, Volume 110, Issue A1, CiteID A01109

Physics

5

Interplanetary Physics: Coronal Mass Ejections (7513), Interplanetary Physics: Ejecta, Driver Gases, And Magnetic Clouds, Interplanetary Physics: Interplanetary Shocks, Interplanetary Physics: Solar Wind Plasma

Scientific paper

We report interplanetary scintillation (IPS) measurements made by the 327 MHz four-station system of the Solar-Terrestrial Environment Laboratory of Nagoya University, during 21 October to 8 November 2003. In this period, solar activity increased greatly owing to the appearance of huge eruptive sunspots on the solar disk. Interplanetary (IP) disturbance events traveling from the Sun beyond the Earth's orbit have been detected clearly from our IPS observations in association with most of the major eruptive events that occurred on the Sun during that period. A possible link between solar/IPS events and near-Earth (IP shock) events in that same period was investigated in this study. As a result, an IP counterpart was identified by our IPS observations for all of the shock events which occurred during the period, and the link to solar events was established unambiguously for the majority of shock events on the basis of the identification of their IP counterparts. Among the IP disturbance events, the most prominent one occurred between 28 and 29 October 2003, and it is considered as an IP counterpart to the 28 October X17 flare event. Our IPS data revealed a complex feature of this IP disturbance and demonstrated that the global distribution of the solar wind density turbulence settled into a rather quiescent condition after the X17 event except between 2 and 4 November 2003, despite the occurrence of marked solar activities. This is in clear contrast to the fact that enhancements of the turbulence level had taken place frequently before the event. The lack of marked g-value enhancements for those events is considered partly due to the intrinsic effect related to a change in the global distribution of the solar wind turbulence and partly due to artificial effects inherent in our IPS observations. The radial expansion of the IP disturbance was tracked successfully by consecutive IPS observations during the period between 2 and 4 November in association with the 2 November X8.3 flare event. The movement of this IP disturbance inferred from IPS data was found to be generally consistent with the average transit speed of the IP shock associated with the X8.3 event, although some deceleration of the IP disturbance may have taken place.

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