Simulations of coronal shock acceleration in self-generated turbulence
Simulations of coronal shock acceleration in self-generated turbulence
复制标题
自生湍流中日冕冲击加速度的模拟
DOI：
10.1016/j.jastp.2007.08.064
复制
发表时间：
2008
影响因子：
1.9
通讯作者：
T. Laitinen
中科院分区：
文献类型：
--
作者：
R. Vainio;T. Laitinen
我们最近提出了一个数值模型来模拟高能粒子在日冕冲击波中的加速和传输，其中包括高能粒子对Alfvén波的反作用，Alfvén波负责它们在环境介质中的散射[Vainio，R.，Laitinen，T.，2007.自生湍流中日冕扩散激波加速的蒙特卡罗模拟。Astrophysical Journal 658，622-630].模型的结果意味着，高能质子加速到超过100兆电子伏的能量可以发生在几分钟内在平行的日冕冲击驱动的快速日冕物质抛射。在本文中，我们给出了一个详细的描述的数值模型及其预见的扩展。我们扩展了第一篇论文中提出的参数研究，以涵盖（较短和）较长的时间尺度，并提出了在SEP事件的初始阶段在行星际介质中观察到的强度。我们还研究了自洽计算的散射平均自由程。最后，该模型解释离子加速到相对论能量的潜力进行了讨论。
We have recently presented a numerical model to simulate the acceleration and transport of energetic particles at coronal shock waves, which includes the back-reaction of the energetic particles on the Alfvén waves responsible for their scattering in the ambient medium [Vainio, R., Laitinen, T., 2007. Monte Carlo simulations of coronal diffusive shock acceleration in self-generated turbulence. Astrophysical Journal 658, 622–630]. The model results imply that the acceleration of energetic protons to energies exceeding 100 MeV can occur in some minutes in parallel coronal shocks driven by fast CMEs. In this paper we give a detailed description of the numerical model and its foreseen extensions. We extend the parameter study presented in the first paper to cover (shorter and) longer time scales, and present the intensities observed in the interplanetary medium during the initial phases of an SEP event. We also study the scattering mean free path resulting from the self-consistent computations. Finally, the potential of the model to explain ion acceleration up to relativistic energies is discussed.