Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh41a1894l&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH41A-1894
Physics
[2104] Interplanetary Physics / Cosmic Rays, [2114] Interplanetary Physics / Energetic Particles
Scientific paper
Quiet-time enhancements at 1 AU of MeV electrons that originate at Jupiter have been observed for decades. Often the intensities show a ~27-day variation in their amplitude, superposed on the ~13-month Jovian synodic period. Various contributing factors have been suggested as the cause of the 27-day variations. One possibility is that transport effects such as diffusion barriers produced by co-rotating interaction regions (CIRs) periodically hinder the transport of electrons between Jupiter and the observer. Also, intensity variations might arise at different solar wind speeds as the magnetic connection of the observer to Jupiter changes. A third possibility, rather than transport effects, is variations in the source strength itself, as might happen if CIRs or high-speed solar wind streams periodically stimulate electron release from the Jovian magnetosphere. Particles measured by the High Energy Telescope (HET) on the twin STEREO spacecraft include electrons from ~0.7 to 4 MeV, and Jovian electrons are clearly observed in this instrument. With the two STEREO spacecraft widely separated in longitude, they are often in different solar wind streams or on opposite sides of a CIR. By comparing the phase of the Jovian electron intensity variations measured by STEREO/HET at the two locations, we assess whether transport effects or source intensity changes are the dominant cause of their 27-day variations.
Cummings Alan C.
Leske Richard A.
Mewaldt Richard A.
Stone Edward C.
von Rosenvinge Tycho T.
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