Observations of Solar Energetic Particle Events over the Polar Regions of the Sun at Solar Maximum with the Ulysses COSPIN High Energy Telescope and IMP-8*

Details Observations of Solar Energetic Particle Events over the Polar Regions of the Sun at Solar Maximum with the Ulysses COSPIN High Energy Telescope and IMP-8* Observations of Solar Energetic Particle Events over the Polar Regions of the Sun at Solar Maximum with the Ulysses COSPIN High Energy Telescope and IMP-8*

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52b..06m&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH52B-06

Other

7519 Flares, 2118 Energetic Particles, Solar

Scientific paper

The High Energy Telescope (HET) of the Ulysses COSPIN experi-ment measures intensities and spectra of solar energetic particles (SEPs) with good energy and charge resolution at energies above ~30 MeV/n. During the recent passes over the north and south polar re-gions of the sun, Ulysses observed a number of solar energetic particle events associated with solar activity at low latitudes. Where IMP-8 observations were available, all SEP events observed at proton energies >~30 MeV by Ulysses in the polar regions (solar latitudes above 70 degrees) were also observed at IMP-8. HOwever peak intensities were generally lower and the onsets and rises to maximum were in general significantly slower at Ulysses than at IMP. Anisotropies during the onsets of SEP events at Ulysses were in almost all cases directed outward along the nominal Parker spiral interplanetary magnetic field, implying that the source of the particles on the field lines connecting to Ulysses was inside the orbit of Ulysses. In the late stages of events, generally four to five days after onset, particle fluxes at IMP and Ulysses were approximately equal and remained so for the remainder of the decay phase. We will summarize these and other results from both the north and south polar passes and discuss their significance for models of the ac-celeration and propagation of solar energetic particles. * This work was supported in part by NASA Contract JPL-955432 and by NASA Grant NAG5-8032.

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