Modeling of the Heliospheric Interface, Magnetic Field, and Cosmic-Ray Transport
Modeling of the Heliospheric Interface, Magnetic Field, and Cosmic-Ray Transport
复制标题
日光层界面、磁场和宇宙射线传输的建模
DOI：
--
复制
发表时间：
2007
期刊：
影响因子：
--
通讯作者：
K. Scherer
中科院分区：
文献类型：
--
作者：
S. Ferreira;M. Potgieter;K. Scherer
本文研究了局部天体层中的磁化流和宇宙线输运。一个混合的数值模型被用来计算日光层界面，日光层磁场，和宇宙射线调制。假设输运参数与磁场成反比，则内日鞘中的场的放大导致这些参数在激波上突然减小。这一点，再加上我们的模型计算表明，压缩和加热的太阳风流在激波后区域不是无发散的，导致了日鞘中宇宙射线粒子的有效绝热加速。特别是，计算出的异常粒子的峰值不是在激波处，而是在离内日鞘一定距离的地方，在那里这个区域充满了相对高强度的加热异常粒子。然而，这种影响在很大程度上取决于日鞘中的传输参数的值。它还表明，在运动学传输的日光层磁场的改善导致一个显着不同的空间分布的宇宙射线相比，帕克模型。
Magnetized flow and cosmic-ray transport in the local astrosphere are studied. A hybrid numerical model is used to calculate the heliospheric interface, the heliospheric magnetic field, and cosmic-ray modulation. Assuming that the transport parameters scale inversely proportional to the magnetic field, the amplification of the field in the inner heliosheath results in a sudden decrease of these parameters over the shock. This, together with our model calculations showing the compressed and heated solar wind flow is not divergence-free in the postshock region, results in effective adiabatic acceleration of cosmic-ray particles in the heliosheath. In particular, the peak of the computed anomalous particles is not at the shock but some distance into the inner heliosheath, where this region becomes populated with relatively high intensities of heated anomalous particles. However, this effect is largely dependent on the values of the transport parameters in the heliosheath. It is also shown that an improvement in the kinematically transported heliospheric magnetic field leads to a significantly different spatial distribution of cosmic rays compared to a Parker model.