Identification of Interplanetary Coronal Mass Ejections at Ulysses Using Multiple Solar Wind Signatures, and Comparison with ICMEs Observed at the Earth and in the Inner Heliosphere

Details Identification of Interplanetary Coronal Mass Ejections at Ulysses Using Multiple Solar Wind Signatures, and Comparison with ICMEs Observed at the Earth and in the Inner Heliosphere Identification of Interplanetary Coronal Mass Ejections at Ulysses Using Multiple Solar Wind Signatures, and Comparison with ICMEs Observed at the Earth and in the Inner Heliosphere

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh13b1979r&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH13B-1979

Physics

[2101] Interplanetary Physics / Coronal Mass Ejections, [2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [2162] Interplanetary Physics / Solar Cycle Variations, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

In previous studies, we have discussed the identification of interplanetary coronal mass ejections (ICMEs) near the Earth based on various solar wind signatures, in particular anomalously low solar wind proton temperatures and plasma compositional/charge state anomalies relative to the composition of the ambient solar wind. We apply similar methods to observations from the Ulysses spacecraft that was launched in 1990 into a heliocentric orbit over the poles of the Sun. Some 270 probable ICMEs are identified during the spacecraft mission, which ended in 2009. We compare the properties of the ICMEs detected at Ulysses with those observed near the Earth and in the inner heliosphere by the Helios spacecraft.

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