Shock Acceleration of Solar Energetic Protons: The First 10 Minutes | Zendy

C. K. Ng | Zendy; D. V. Reames | Zendy

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Shock Acceleration of Solar Energetic Protons: The First 10 Minutes

Author(s) -

C. K. Ng,

D. V. Reames

Publication year - 2008

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/592996

Subject(s) - physics , acceleration , fermi acceleration , shock wave , proton , shock (circulatory) , solar flare , plasma , astrophysics , solar wind , atomic physics , fermi gamma ray space telescope , particle acceleration , shock waves in astrophysics , coronal mass ejection , computational physics , nuclear physics , mechanics , classical mechanics , medicine

Proton acceleration at a parallel coronal shock is modeled with self-consistent Alfven 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 r☉, for typical coronal conditions and low ambient wave intensities. Interaction of high-energy protons of large pitch angles with Alfven 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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