Shock Acceleration of Solar Energetic Protons: The First 10 Minutes

Details Shock Acceleration of Solar Energetic Protons: The First 10 Minutes Shock Acceleration of Solar Energetic Protons: The First 10 Minutes

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...686l.123n&link_type=abstract

The Astrophysical Journal, Volume 686, Issue 2, pp. L123-L126.

Astronomy and Astrophysics

Astronomy

12

Acceleration Of Particles, Shock Waves, Sun: Coronal Mass Ejections (Cmes), Sun: Particle Emission

Scientific paper

Proton acceleration at a parallel coronal shock is modeled with self-consistent Alfvén wave excitation and shock transmission. 18-50 keV seed protons at 0.1% of plasma proton density are accelerated in 10 minutes to a power-law intensity spectrum rolling over at 300 MeV by a 2500 km s-1 shock traveling outward from 3.5 rsolar, for typical coronal conditions and low ambient wave intensities. Interaction of high-energy protons of large pitch angles with Alfvén waves amplified by low-energy protons of small pitch angles is key to rapid acceleration. Shock acceleration is not significantly retarded by sunward streaming protons interacting with downstream waves. There is no significant second-order Fermi acceleration.

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