Physics – Plasma Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh41c..02d&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH41C-02
Physics
Plasma Physics
[2101] Interplanetary Physics / Coronal Mass Ejections, [2114] Interplanetary Physics / Energetic Particles, [2139] Interplanetary Physics / Interplanetary Shocks, [7867] Space Plasma Physics / Wave/Particle Interactions
Scientific paper
Coronal Mass Ejection- or CME-driven interplanetary (IP) shocks are responsible for causing the so-called energetic storm particle (ESP) events observed at Earth. However, despite recent observational and theoretical advances, many important questions regarding such CME-associated particle events remain unanswered. This is because ESP events occur due to a confluence of numerous poorly understood physical effects all of whose contributions can vary with time and location. These include: the origin, structure, and obliquity of the shocks, the nature of wave-particle interactions and the type of turbulence that is present near the shocks, the distribution and composition of the seed populations, and the type of injection and acceleration processes involved. In this paper, we combine observations of ~0.1-0.5 MeV/nucleon O and Fe ions with that of the magnetic field near 17 CME-driven IP shocks observed at the Advanced Composition Explorer and Wind spacecraft to study the temporal evolution of (1) O and Fe intensities, (2) power-law spectral indices of O, (3) the Fe/O ratios, and (4) the magnetic field power spectrum. In particular, we identify unique signatures that differentiate between shocks where the seed population is dominated by low-energy (<100 keV/nucleon) suprathermal ions and those events where it is dominated by suprathermal-through-energetic seed ions with spectra extending at least up to ~0.5 MeV/nucleon. Such observational signatures may also be useful in modeling the properties of the so-called large gradual solar energetic particle (SEP) events that are primarily accelerated by CME shocks near the Sun.
Dayeh M. A.
Desai Mihir I.
Kasper Justin Christophe
Lee Martin A.
Mason Glenn M.
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