TESTING TRANSPORT THEORIES WITH SOLAR ENERGETIC PARTICLES
TESTING TRANSPORT THEORIES WITH SOLAR ENERGETIC PARTICLES
复制标题
用太阳能粒子测试输运理论
DOI：
10.1088/0004-637x/693/1/69
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发表时间：
2009
期刊：
影响因子：
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通讯作者：
Y. Kartavykh
中科院分区：
文献类型：
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作者：
W. Dröge;Y. Kartavykh
太阳粒子事件的详细建模提供了推导描述高能粒子在内日球层传播的系数的可能性，例如散射平均自由程，从而测试粒子与磁场波动相互作用的不同理论的有效性。此外，还可以获得有关波动的三维结构和动力学性质的信息，并与直接磁场观测的结果进行比较。我们采用不同的方法对标准理论和动态准线性理论计算的俯仰角扩散系数的聚焦输运方程进行了数值求解，并研究了100 keV电子和MeV质子的俯仰角分布。我们发现，从包含动态准线性理论的模型中预测电子的俯仰角分布，并假设波动由20%的平板和80%的二维分量组成，与质子的预测有很大不同。与2000年2月18日太阳事件的粒子观测结果的比较表明，这些预测也与观测到的电子俯仰角分布存在强烈的分歧。我们的研究结果表明，尽管上述模型最近成功地从太阳风湍流观测中对平行于平均磁场的粒子散射平均自由程进行了定量正确的预测，但仍然不完整。
The detailed modeling of solar particle events offers the possibility of deriving coefficients describing the propagation of energetic particles in the inner heliosphere such as scattering mean free paths and thus to test the validity of different theories for the interaction of the particles with magnetic field fluctuations. In addition, information about the three-dimensional structure and the dynamical properties of the fluctuations can be obtained and compared with results from direct magnetic field observations. We apply different methods to numerically solve the focused transport equation for pitch angle diffusion coefficients calculated from standard and dynamical quasi-linear theory, and investigate the resulting pitch angle distributions for 100 keV electrons and for MeV protons. We find that pitch angle distributions predicted for electrons from a model comprising dynamical quasi-linear theory and the assumption that the fluctuations are composed of a 20% slab and an 80% two-dimensional component differ significantly from those predicted for protons. A comparison with particle observations from the solar event of 2000 February 18 reveals that these predictions are also in strong disagreement with the observed electron pitch angle distributions. Our findings indicate that the above model, inspite of its recent success in making quantitatively correct predictions for the particle's scattering mean free path parallel to the average magnetic field from observations of solar wind turbulence, is still not complete.