Cosmic Ray Observations During the October-November 2003 Storms With Spaceship Earth and the Muon Detector Network

Details Cosmic Ray Observations During the October-November 2003 Storms With Spaceship Earth and the Muon Detector Network Cosmic Ray Observations During the October-November 2003 Storms With Spaceship Earth and the Muon Detector Network

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh33a..05m&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH33A-05

Physics

2118 Energetic Particles, Solar, 2139 Interplanetary Shocks, 7513 Coronal Mass Ejections, 7519 Flares

Scientific paper

A series of very large relativistic solar proton events occurred in October-November 2003. During this period, many instruments observed events associated with this solar activity, such as large geomagnetic storms, cosmic ray ground level enhancements (GLE) and Forbush decreases. The global network of high energy cosmic ray observatories on Earth is able to measure precisely temporal variations of cosmic ray streaming (the anisotropy of intensity) from those events. We use data of the 11-station ``Spaceship Earth'' network of high-latitude neutron monitors and the ground-based muon detector network to analyze three types of anisotropies: Loss cone, bidirectional streaming, and B×∇ n. Loss cone anisotropy is a cosmic ray intensity deficit in the small pitch angle region. This anisotropy may exist ~10% of an interplanetary scattering mean free path ahead of the shock front, which implies that it may be observed as a precursor of the CME shock impacting Earth. Bidirectional streaming is a type of second order anisotropy and indicates the presence of ejecta around Earth. The B×∇ n anisotropy is produced from density (n) gradients associated with the cosmic ray depleted region in and near the CME. This anisotropy allows us to deduce the near-Earth trajectory of the ejecta. We will report temporal variations of anisotropies and discuss precursor anisotropies, bidirectional streaming, and the orientation of ejecta for each storm event during this solar high activity period. This work is supported in part by U.S. NSF grants ATM-0207196 and ATM-0000315 and in part by the joint research program of the Solar-Terrestrial Environment Laboratory, Nagoya University.

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