Energetic Particle Observations During the Ulysses Fast Latitude Scan

Details Energetic Particle Observations During the Ulysses Fast Latitude Scan Energetic Particle Observations During the Ulysses Fast Latitude Scan

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52b..05s&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH52B-05

Physics

7514 Energetic Particles (2114)

Scientific paper

Peak/National Solar Observatory show that during the second Ulysses fast latitude scan, the sun's magnetic dipole was oriented more or less perpendicular to the spin axis (with at times a significant quadrupole component) and that the current sheet was highly tilted. This configuration is ideal for the formation of stream interaction regions in the solar wind. Using particle intensity profiles and anisotropy measurements over a wide range of energies from the COSPIN instrument, and magnetic field and plasma observations, we identify the magnetic structures in the heliosphere which are a consequence of the magnetic field configuration on the Sun. We show that the heliosphere contained many co-rotating interaction regions, stable only for a few rotations. The many solar flares and CME's give rise to many injections of highly energetic SEP particles. We identify CIR's and CME's which locally accelerate the energetic particles. We show that during the fast latitude scan, the heliosphere was filled by a complicated mix of CME and CIR accelerated particles. When the solar activity was high, the particle population was dominated by CME-accelerated particles, but when activity was low, CIR accelerated particles Magnetic field observations from the Wilcox Solar Observatory and coronal hole observations from the Kitt dominated.

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