Corotating interaction regions during the solar cycle 22 and 23 minima

Details Corotating interaction regions during the solar cycle 22 and 23 minima Corotating interaction regions during the solar cycle 22 and 23 minima

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh14a..03b&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH14A-03

Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

Corotating interaction regions (CIRs) are the outcome of the interaction of two types of plasma structures in the solar corona: fast, low-density, high-temperature streams that originate at high latitudes and slow streams that originate near the solar equator. As a result of the Sun's rotation, the interaction regions form spiral structures that corotate with the Sun. Clearly distinguishable fast and slow wind streams are usually observed near solar minima. Using Ulysses observations, we have identified solar wind parameters corresponding to the solar cycle 22 and 23 minima. We present high-resolution results on the CIR evolution, formation of forward and reverse shocks, development of corotating merged interaction regions, and their transmission through the termination shock and propagation in the heliosheath. Numerical results are compared with the Ulysses and Voyager observations.

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