Extended Injection Histories of Near-Relativisitic Solar Electrons and Their Relation to SEP Ion Events

Details Extended Injection Histories of Near-Relativisitic Solar Electrons and Their Relation to SEP Ion Events Extended Injection Histories of Near-Relativisitic Solar Electrons and Their Relation to SEP Ion Events

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh11d1138h&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH11D-1138

Physics

Plasma Physics

2100 Interplanetary Physics, 2114 Energetic Particles, Heliospheric (7514), 6200 Planetology: Solar System Objects (New Field), 7500 Solar Physics, Astrophysics, And Astronomy, 7800 Space Plasma Physics

Scientific paper

Energetic solar electrons provide important information on the acceleration and release of all classes of solar energetic particles (SEPs). The relationships of their intensities to ion abundances and isotopic composition (e.g., 3He/4He) have been studied for decades. Their near-light speed and nearly scatter-free propagation out to 1AU preserve many details of their injection into the solar wind. Recently we have been exploiting the high timing and angular resolution of the ACE/EPAM measurements of 38-315 keV electrons [Haggerty and Roelof, ApJ., 579, 841, 2002]. We now are able to reconstruct the injection histories of beam-like electrons extending well into the SEP events. This is accomplished by subtracting out the back-scattered electrons that have returned from magnetic irregularities beyond 1 AU, mirrored inside 1AU, and then returned to 1AU. The difference between the total outgoing intensity and that of this mirrored component (time delayed) gives the intensity of the electrons that are still arriving directly from the Sun. The mathematical relation is js(μ ,t-s/v)=j(μ ,t)-j(-μ ,t-2τ ), where μ is the pitch cosine (measured positive anti-sunwards), s is the trajectory distance traveled at velocity v, and τ is the time for a particle with pitch cosine μ <0 at 1AU to reach its mirroring point inside 1AU. We find that the injection of solar electrons often lasts for considerably more than an hour at significant intensities. This analysis yields new diagnostics of the acceleration/release process, which we have ascribed to CME-associated shock acceleration [Simnett, Roelof, and Haggerty, ApJ, 579, 854, 2002]. The relation of electron injection to ion injection and 3He/4He variations is the subject of an ongoing joint study [Mewaldt et al., 28thICRC, SH1.3, 17, 2003].

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