HR: 1340h
AN: SH33A-1090    [Abstracts]
TI: Multipoint Observations of Stream Interaction Regions
AU: * Jian, L K
EM: jlan@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics; Department of Earth and Space Sciences; University of California, Los Angeles, 595 Charles E. Young Dr. East, 6862 Slichter Hall, Los Angeles, CA 90095, United States
AU: Russell, C T
EM: ctrussel@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics; Department of Earth and Space Sciences; University of California, Los Angeles, 595 Charles E. Young Dr. East, 6862 Slichter Hall, Los Angeles, CA 90095, United States
AU: Luhmann, J G
EM: jgluhman@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, Berkeley, CA 94720, United States
AU: Skoug, R M
EM: rskoug@lanl.gov
AF: Space Science and Applications; Los Alamos National Laboratory, Group ISR-1, MS D466, Los Alamos, NM 87545, United States
AU: Steinberg, J T
EM: jsteinberg@lanl.gov
AF: Space Science and Applications; Los Alamos National Laboratory, Group ISR-1, MS D466, Los Alamos, NM 87545, United States
AU: Galvin, A B
EM: toni.galvin@unh,edu
AF: Institute for the Study of Earth, Oceans, and Space; Department of Physics Astrophysics, University of New Hampshire, Morse Hall, 39 College Road, Durham, NH 03824-3525, United States
AB: A stream interaction region (SIR) forms when a fast stream overtakes a preceding slow stream. These SIR structures continue to evolve as they move away from the Sun. During short intervals of Ulysses' perihelion and aphelion passes, Ulysses was at almost the same helio-latitude as ACE and Wind, and the three spacecraft observed several of the same SIRs. Based on multipoint observations of the same events, we study the evolution of SIR properties over a relatively large temporal and spatial scale. In particular, we examine the associated shock, duration, width, total perpendicular pressure, magnetic field and velocity variation, and compare them with our previous statistical results of SIR evolution from 1 to 5.3 AU. We also compare the observations of STEREO and ACE, to study the structures of SIRs and their evolution over shorter spatial and temporal scales.
DE: 2102 Corotating streams
DE: 2134 Interplanetary magnetic fields
DE: 2139 Interplanetary shocks
DE: 2162 Solar cycle variations (7536)
DE: 2164 Solar wind plasma
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting