Solar Energetic Particles Near the Orbit of Jupiter From the Oct/Nov. 2003 Solar Events: Observations From the Ulysses COSPIN Instruments

Details Solar Energetic Particles Near the Orbit of Jupiter From the Oct/Nov. 2003 Solar Events: Observations From the Ulysses COSPIN Instruments Solar Energetic Particles Near the Orbit of Jupiter From the Oct/Nov. 2003 Solar Events: Observations From the Ulysses COSPIN Instruments

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh33a..04m&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH33A-04

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2118 Energetic Particles, Solar

Scientific paper

During the period of intense solar activity in October/November 2003, Ulysses was a little more than 5.2 AU from the Sun, and between about 4 and 6 degrees North of the heliographic equator. During the same period its heliographic longitude with respect to Earth decreased by about 1 degree per day starting from ~128 degrees west of Earth on Oct. 22 (day 295), when the large active region No. 486 rotated onto the face of the Sun. Exceptionally strong solar activity began with an X17 flare having an X-ray maximum at 1110 on Oct. 28 (Day 301), and continued at least through Nov. 4 (Day 308), when an X28 flare occurred near the Sun's west limb. Protons with energy >40 MeV from the Oct. 28 event had clearly begun to arrive at Ulysses by 2300 UT, showing a rapid increase in intensity and strong outward flow along the interplanetary magnetic field. At energies of ~2-4 MeV, proton intensities, already somewhat elevated, showed a clear and abrupt increase, also with strong particle flow outward along the field, several hours earlier at about 1700 UT, while ~5-10 MeV electrons showed a very minor increase in intensity starting about 2300 UT, but did not show a large increase (again with outward flow) until ~0600 UT on Oct. 29. For the protons, outward flow along a very quiet magnetic field persisted during a smooth decay (at high energies) and during a period with little intensity change (at low energies) until Nov. 7 (day 311). Other large X-class flares observed on Oct. 29, Nov. 2, and the X28 on Nov. 4, all of which produced significant particle flux increases at 1 AU, produced no clear increases in the particle fluxes at Ulysses. A second onset with a much softer energy spectrum began on Nov. 8 and continued through a period of disturbed magnetic structure until Nov. 14 (day 318) when a rapid decrease in intensity of the high-energy particles began. The decrease was associated with a progressive increase in solar wind speed towards the maximum of ~1000 km/s observed on Nov. 15. We will present a comprehensive report of the particle intensities, spectra, and anisotropies from the COSPIN energetic particle telescopes, and will attempt to relate them to the evolving interplanetary disturbances initiated by the solar events. The instruments provide measurements over a proton energy range from ~0.3 MeV up to GeV energies, and for electrons from a few MeV up to >100 MeV

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