Interplanetary CME Effects on the Short-Period Variability in the GCR Flux

Details Interplanetary CME Effects on the Short-Period Variability in the GCR Flux Interplanetary CME Effects on the Short-Period Variability in the GCR Flux

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh22a..08m&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH22A-08

Physics

Plasma Physics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7859] Space Plasma Physics / Transport Processes, [7924] Space Weather / Forecasting

Scientific paper

We examine several cases of short-period variability in the GCR flux in the solar wind and in the magnetosphere using background channels in several spacecraft including Polar, ACE, and INTEGRAL. INTEGRAL in particular offers unprecedented resolution of Forbush decreases with GCR count rates exceeding 10^5 counts/s. We find correlations between the GCR fine scale structure and the local solar wind magnetic field topology. Often these periods occur in and around the time of the passage of an interplanetary coronal mass ejection (ICME) and its substructures. The fine structures in the GCR intensities along with the Forbush decrease caused by the ICME are propagated outward with very little change from L1 to the Earth indicating that parcels of solar wind are transporting the GCR population outward in the heliosphere. This solar wind convection of GCR fine structure is observed for both increases and decreases in GCR intensity and the fine-structure increases and decreases are bracketed by solar wind magnetic field discontinuities within the ICME. Similar to the dispersionless modulation of the electron heat flux, which is an indicator of changes in magnetic field topology, the fine structures in the GCR observations show that the intensity levels in the GCR flux may undergo a similar partitioning associated with local changes observed in the interplanetary magnetic field. We also find this local field topology affects the energetic electron population (>500 keV) in the magnetosphere and explore such observations in detail. Undoubtedly, the high-resolution measurements made available by the background channels from the INTEGRAL, Polar, and ACE spacecraft give us an unprecedented view into the microphysical processes of energetic particle transport and quite possibly the magnetospheric response to the high frequency content of the interplanetary medium.

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