HR: 08:55h
AN: SH51D-04    [Abstracts]
TI: What mirror mode waves in the solar wind are telling us about the solar corona
AU: * Jian, L
EM: jlan@igpp.ucla.edu
AF: Institute of Geophysics, University of California 405 Hilgard Ave, Los Angeles, CA 90095, United States
AU: Russell, C T
EM: ctrussell@igpp.ucla.edu
AF: Institute of Geophysics, University of California 405 Hilgard Ave, Los Angeles, CA 90095, United States
AU: Luhmann, J G
EM: jgluhman@ssl.berkeley.edu
AF: Space Science Laboratory, University of California, Berkeley, CA 94720, United States
AU: Skoug, R
EM: rskoug@lanl.gov)
AF: Space Science and Laboratory, Los Alamos National Laboratory, Los Alamos, NM 87545, United States
AU: Blanco-Cano, X
EM: xbd@geofisica.unam.mx
AF: Institute of Geophysics, Ciudad Universitaria Coyoacan,Codizo 04510, Mexico D. F., Mexico
AB: We have observed two quite distinct sources of mirror mode waves. Behind the bow shock in the magnetosheath and along the magnetopause, we see mirror mode waves grow from the pressure anisotropy imposed by the shock or the solar wind plasma. We also have observed mirror mode waves in the Saturnian magnetosphere growing from the pressure anisotropy imposed by mass loading from the E-ring torus. These mirror mode waves last a long time and are convected radially away from Saturn. By analogy, the solar wind mirror mode waves could be either generated by shocks or by mass-loading followed by radial transport from the inner corona. We see little evidence in Interplanetary CMEs or the solar wind that these mirror mode waves are caused by shock compressions. We test the radial transport hypothesis by examining the occurrence rate of mirror mode waves in the solar wind at 0.72 AU (with Pioneer Venus Orbiter data), at 1 AU with STEREO, and at 5 AU with Ulysses.
DE: 2101 Coronal mass ejections (7513)
DE: 2134 Interplanetary magnetic fields
DE: 2728 Magnetosheath
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly