IMF Connection for Energetic Protons Observed at ULYSSES via Mid-Latitude Solar Wind Rarefaction Regions

Details IMF Connection for Energetic Protons Observed at ULYSSES via Mid-Latitude Solar Wind Rarefaction Regions IMF Connection for Energetic Protons Observed at ULYSSES via Mid-Latitude Solar Wind Rarefaction Regions

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ssrv...72..309r&link_type=abstract

Space Science Reviews, Volume 72, Issue 1-2, pp. 309-314

Computer Science

11

Heliosphere, Energetic Particles, Corotating High-Speed Streams

Scientific paper

As Ulysses moved inward and southward from mid-1992 to early 1994 we noticed the occasional occurrence of “inter-events”, lasting about 10 days and falling between the recurrent events, observed at proton energies of 0.48 97 MeV, associated with Corotating Interaction Regions (CIR). These inter-events were present for several sequences of two or more solar rotations at intensity levels around 1% of those of the neighbouring main events. When we compared the Ulysses events with those measured on IMP-8 at 1 AU we saw that the inter-events appeared at Ulysses after the extended emission (>10 days) of large fluxes of solar protons of the same energy that lasted at least one solar rotation at 1 AU. The inter-events fell completely within the rarefaction regions (dv/dt<0) of the recurrent solar wind streams. The interplanetary magnetic field (IMF) lines in the rarefactions map back to the narrow range of longitudes at the Sun which mark the eastern edge of the source region of the high speed stream. Thus the inter-events are propagating at mid-latitudes to Ulysses along field lines free from stream-stream interactions. They are seen in the 0.39 1.28 MeV/nucleon He, which exhibit a faster decay, but almost never in the 38 53 keV electrons. We show that the inter-events are unlikely to be accelerated by reverse shocks associated with the CIRs and that they are more likely to be accelerated by sequences of solar events and transported along the IMF in the rarefactions of the solar wind streams.

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