CIR Structures and Their Shocks at ~5AU: Ulysses Fast Latitude Scans

Details CIR Structures and Their Shocks at ~5AU: Ulysses Fast Latitude Scans CIR Structures and Their Shocks at ~5AU: Ulysses Fast Latitude Scans

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh23a1140e&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH23A-1140

Physics

2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2159 Plasma Waves And Turbulence, 2164 Solar Wind Plasma

Scientific paper

Corotating interaction regions (CIRs) are caused by fast stream-slow stream interactions. At large heliocentric distances, they are typically bounded by a pair of fast forward and reverse shocks Ulysses magnetic field and plasma data during fast latitude scans are used to study the structure of CIRs and their shocks as a function of heliolatitude. The fast forward and reverse shock properties (shock normal angles, Mach numbers) bounding CIRs are presented and discussed. What is perhaps most surprising is the complexity of the CIRs at middle latitudes. CIRs do not have the simple "boxcar" shape bounded by fast shocks as previously noted for events detected in the ecliptic plane. The causes of this complexity will be discussed.

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