Fast Shocks From Magnetic Reconnection Outflows

Details Fast Shocks From Magnetic Reconnection Outflows Fast Shocks From Magnetic Reconnection Outflows

2011-04-30

arxiv.org/abs/1105.0120v2

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

Scientific paper

Magnetic reconnection is commonly perceived to drive flow and particle acceleration in flares of solar, stellar, and astrophysical disk coronae but the relative roles of different acceleration mecha- nisms in a given reconnection environment are not well understood. We show via direct numerical simulations that reconnection outflows produce weak fast shocks, when conditions for fast recon- nection are met and the outflows encounter an obstacle. The associated compression ratios lead to a Fermi acceleration particle spectrum that is significantly steeper than the strong fast shocks commonly studied, but consistent with the demands of solar flares. While this is not the only acceleration mechanism operating in a reconnection environment, it is plausibly a ubiquitous one.

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