Modelling of Shock-Accelerated Gamma-Ray Events
Alexandr Afanasiev; Alexis Rouillard; Angels Aran; Blai Sanahuja; David Lario; Jens Pomoell; Olga E. Malandraki; Pietro Zucca; Rami Vainio; Robert Siipola; Suvi Barcewicz
https://urn.fi/URN:NBN:fi-fe2021042720267
Tiivistelmä
Solar γ-ray events recently detected by the Fermi/LAT instrument at energies above 100 MeV have presented a puzzle for solar physicists as many of such events were observed lasting for many hours after the associated flare/coronal mass ejection (CME) eruption. Data analyses suggest the γ-ray emission originate from decay of pions produced mainly by interactions of high-energy protons deep in the chromosphere. Whether those protons are accelerated in the associated flare or in the CME-driven shock has been under active discussion. In this chapter, we present some modelling efforts aimed at testing the shock acceleration hypothesis. We address two γ-ray events: 2012 January 23 and 2012 May 17 and approach the problem by, first, simulating the proton acceleration at the shock and, second, simulating their transport back to the Sun.
Kokoelmat
- Rinnakkaistallenteet [19207]