Physics
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsh51d..04j&link_type=abstract
American Geophysical Union, Spring Meeting 2007, abstract #SH51D-04
Physics
2101 Coronal Mass Ejections (7513), 2134 Interplanetary Magnetic Fields, 2728 Magnetosheath
Scientific paper
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.
Blanco-Cano Xochitl
Jian Li
Luhmann Janet G.
Russell Christopher T.
Skoug Ruth
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