HR: 1340h
AN: SH23A-1140    [Abstracts]
TI: CIR Structures and Their Shocks at ~5AU: Ulysses Fast Latitude Scans
AU: Echer, M P
EM: mariza@dge.inpe.br
AF: Instituto Nacional de Pesquisas Espaciais, Avenida Astronautas 1758, Sao Jose Campos, SP 12227010, Brazil
AU: * Echer, E
EM: eecher@dge.inpe.br
AF: Instituto Nacional de Pesquisas Espaciais, Avenida Astronautas 1758, Sao Jose Campos, SP 12227010, Brazil
AU: Tsurutani, B T
EM: bruce.tsurutani@jpl.nasa.gov
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Guarnieri, F L
EM: guarnieri@univap.br
AF: Universidade do Vale do Paraiba, Urbanova, Sao Jose dos Campos, SP 12227010, Brazil
AB: 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.
DE: 2134 Interplanetary magnetic fields
DE: 2149 MHD waves and turbulence (2752, 6050, 7836)
DE: 2159 Plasma waves and turbulence
DE: 2164 Solar wind plasma
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting