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arXiv 1303.4334astro-ph.SRphysics.space-ph
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减速日冕激波中高能粒子通过自生波的加速

Acceleration of Energetic Particles Through Self-Generated Waves in a Decelerating Coronal Shock

Markus Battarbee, Timo Laitinen, Rami Vainio, Neus Agueda

备注：
5 pages, 8 figures. Copyright (2010) American Institute of Physics. This article may be downloaded for personal use only. Any other use requires prior permission of the author and the American Institute of Physics. The following article appeared in Twelfth International Solar Wind Conference, AIP Conference Proceedings 2010
发表信息：
AIP Conference Proceedings 1216, pp. 84-87, 2010
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摘要：

我们建立了一个日冕冲击波中粒子加速的模拟模型。该模型是基于蒙特卡罗方法，粒子跟踪在规定的大规模电磁场利用引导中心近似。根据准线性理论，颗粒在湍流中散射，散射振幅与回转共振波数处的Alfvén波的强度成正比。阿尔文波与粒子同时被追踪，因此波场从太阳向外传播，使用WKB传播，并补充了唯象波数扩散项和从加速粒子的净通量计算的增长率。我们认为初始波的振幅足够小，以允许快速逃逸的粒子从冲击周围的介质。因此，在我们的模型中，负责粒子扩散加速的阿尔文波是由加速粒子本身产生的。在这项工作中，我们研究了非恒定的冲击波速度和非单调的阿尔文速度对粒子加速方案的影响。我们特别报告如何减速的冲击影响粒子强度和湍流功率的冲击附近的演变。

英文摘要：

We have developed a simulation model of particle acceleration in coronal shock waves. The model is based on a Monte Carlo method, where particles are traced in prescribed large-scale electromagnetic fields utilizing the guiding center approximation. The particles are scattered in the turbulence according to quasilinear theory, with the scattering amplitude directly proportional to the intensity of Alfvén waves at gyro-resonant wavenumbers. The Alfvén waves are traced simultaneously with the particles, so that the wave field is propagated outwards from the Sun using WKB propagation supplemented with a phenomenological wavenumber diffusion term and a growth rate computed from the net flux of the accelerated particles. We consider initial wave amplitudes small enough to allow rapid escape of particles from the shock to the ambient medium. Thus, in our model the Alfvén waves responsible for the diffusive acceleration of particles are generated by the accelerated particles themselves. In this work, we study the effects of non-constant shock velocity and non-monotonic Alfvén velocity on particle acceleration scenarios. We report in particular how the deceleration of a shock affects particle intensity and turbulence power evolution in the vicinity of the shock.

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