Remote Sensing of Particle Acceleration at the Sun

Details Remote Sensing of Particle Acceleration at the Sun Remote Sensing of Particle Acceleration at the Sun

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh42a..02s&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH42A-02

Physics

7514 Energetic Particles (2114), 7519 Flares, 7554 X-Rays, Gamma Rays, And Neutrinos, 7594 Instruments And Techniques

Scientific paper

The Solar Sentinels Mission offers the opportunity for in-situ and remote observations of particles accelerated in the vicinity of the Sun. The proximity to the Sun and observations from several vantage points will minimize transport effects in determining the characteristics of the particle population escaping the Sun from the in-situ observations. Remote observations of gamma rays and neutrons with instruments on the Sentinels will provide information on the population of particles that interact at the Sun. Most of these particles interact in footpoints after transport in closed magnetic loops. At present we do not know the relationship between the acceleration processes that accelerate these particles and those that accelerate solar energetic particles observed in space. Observations of the 2005 January 20 solar flare by RHESSI provide information on a flare that appears to comprise two episodes of particle acceleration: one producing a particle population that interacts in footpoints and has a spectral index of ~ 3 for an assumed power-law spectrum; and a second one producing a much harder spectrum, index ≤ 2.3, lasting for about 2 hours, whose impact sites on the Sun are unknown. The gamma rays from this hard component are dominated by pion-decay emission measured both by RHESSI and Coronas. The rise time and spectral hardness of this latter component appear to be similar to those of particles observed in the ground level event and in space. Launch of the AGILE and GLAST observatories in 2007 provide the capability for high-energy gamma ray observations over the next several years and will complement the lower-energy observations made by Sentinels launched during Solar Cycle 24. This work is supported by NASA SEC-GI and SR&T grants.

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