Stochastic Re-Acceleration of Protons in the Downstream Region of a Coronal Shock

Details Stochastic Re-Acceleration of Protons in the Downstream Region of a Coronal Shock Stochastic Re-Acceleration of Protons in the Downstream Region of a Coronal Shock

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh34a..02a&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH34A-02

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles

Scientific paper

Recent SDO/AIA observations of CME in the low corona have finally confirmed the formation of coronal shock waves in the low corona. This supports the viability of shock acceleration as the mechanism for the genesis of large gradual SEP events. However, a careful analysis of observational data of the early phases of large SEP events indicates that it might be hard to understand some of the spectral characteristics at deca-MeV energies in detail relying on a model of diffusive shock acceleration alone. We have recently presented a test-particle model where coronal shock acceleration and stochastic re-acceleration in the shock downstream region can account for the hard spectral features in the deca-MeV range. The problem of a test-particle calculation in the case of stochastic acceleration is, however, that a time-stationary wave field acts as an infinite energy reservoir for the particles being accelerated by turbulence. To account for this problem, we employ our self-consistent wave-particle interaction simulation code to compute the evolution of the wave frequency and proton energy spectra in the downstream region of a coronal shock. Parameter space allowed by different types of turbulence generation models is explored and regions favorable to explaining the proton energy spectra in large gradual events are identified.

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