Solar wind collimation of the Jupiter high velocity dust streams

Details Solar wind collimation of the Jupiter high velocity dust streams Solar wind collimation of the Jupiter high velocity dust streams

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p41c1307f&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P41C-1307

Physics

2129 Interplanetary Dust, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 6213 Dust, 6220 Jupiter

Scientific paper

The dust bursts discovered by the Ulysses dust sensor when approaching Jupiter in 1992 were later confirmed as collimated streams of high velocity (~200 km/s) charged (~5V) dust grains escaping from Jupiter and dominated by the interplanetary Magnetic field (IMF). With Cassini, a similar phenomenon was observed in Saturn. It was demonstrated that the Jovian dust streams are closely related to the solar wind compressed regions, either Corotating interaction regions (CIRs) or Coronal mass ejections (CMEs) ¨Cto a minor extent-. Actually the dust streams seem ultimately to be generated by such events. This can be explained considering that dust grains are accelerated as they gain substantial energy while compressed at the forward and reverse shocks that bound or precede these solar wind regions.

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