A NUMERICAL SIMULATION OF COSMIC RAY MODULATION NEAR THE HELIOPAUSE. II. SOME PHYSICAL INSIGHTS
A NUMERICAL SIMULATION OF COSMIC RAY MODULATION NEAR THE HELIOPAUSE. II. SOME PHYSICAL INSIGHTS
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日球层顶附近宇宙射线调制的数值模拟。
DOI：
10.3847/0004-637x/826/2/182
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发表时间：
2015-07
影响因子：
4.9
通讯作者：
Strauss R. du Toit
中科院分区：
文献类型：
--
作者：
Luo Xi;Potgieter Marius S.;Zhang Ming;Pogorelov Nikolai V.;Feng Xueshang;Strauss R. du Toit
用混合输运模型研究了宇宙线在太阳顶层(HP)附近的输运，其参数受旅行者1号航天器观测的约束。我们模拟了日光层中不同方向的CR径向通量。太阳风区域和星际区域之间沿着日光层的尾部和极地方向没有明确的薄层。通过分析沿旅行者2号方向的径向通量曲线，结合其轨迹信息，预测旅行者2号穿越高压线的时间为2017.14。我们模拟了沿旅行者1号方向不同能量值的CR径向通量。我们发现，在HP之外只有一个约10Au宽的适度调制区域，因此旅行者1号观测星际局域光谱在数值模拟中是合理的。我们分析了随机数值(时间倒退)方法中的伪粒子的出射信息，推测它们代表了CR粒子的行为，我们发现从鼻部追踪到的伪粒子存在于尾部区域。这意味着许多CR粒子直接从日球层尾部扩散到高压附近的鼻部区域。此外，当从星际局部介质(LISM)追踪伪粒子时，发现它们从模拟区域的出口位置(真实粒子的入口)沿着规定的星际磁场方向。这表明平行扩散在LISM中主导了CR粒子的输运。
Cosmic ray (CR) transport near the heliopause (HP) is studied using a hybrid transport model, with the parameters constrained by observations from the Voyager 1 spacecraft. We simulate the CR radial flux along different directions in the heliosphere. There is no well-defined thin layer between the solar wind region and the interstellar region along the tail and polar directions of the heliosphere. By analyzing the radial flux curve along the direction of Voyager 2, together with its trajectory information, the crossing time of the HP by Voyager 2 is predicted to be in 2017.14. We simulate the CR radial flux for different energy values along the direction of Voyager 1. We find that there is only a modest modulation region of about 10 au wide beyond the HP, so that Voyager 1 observing the Local Interstellar Spectra is justified in numerical modeling. We analyze the heliospheric exit information of pseudo-particles in our stochastic numerical (time-backward) method, conjecturing that they represent the behavior of CR particles, and we find that pseudo-particles that have been traced from the nose region exit in the tail region. This implies that many CR particles diffuse directly from the heliospheric tail region to the nose region near the HP. In addition, when pseudo-particles were traced from the Local Interstellar Medium (LISM), it is found that their exit location (entrance for real particles) from the simulation domain is along the prescribed Interstellar Magnetic Field direction. This indicates that parallel diffusion dominates CR particle transport in the LISM.
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影响因子：
2.6
作者：
R. D. Strauss;M. Potgieter
通讯作者：
R. D. Strauss;M. Potgieter
日球层顶附近宇宙射线调制的数值模拟
影响因子：
4.9
作者：
Luo Xi;Zhang Ming;Potgieter Marius;Feng Xueshang;Pogorelov N. V.
通讯作者：
Pogorelov N. V.
影响因子：
64.8
作者：
E. Stone;A. Cummings;F. Mcdonald;B. Heikkila;N. Lal;W. Webber
通讯作者：
E. Stone;A. Cummings;F. Mcdonald;B. Heikkila;N. Lal;W. Webber
DOI：
10.1088/0004-637x/782/1/24
发表时间：
2014-01
期刊：
The Astrophysical Journal
影响因子：
--
作者：
J. Kóta;J. Jokipii
通讯作者：
J. Kóta;J. Jokipii
DOI：
10.1088/2041-8205/750/1/l4
发表时间：
2012-05
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
N. Pogorelov;S. Borovikov;G. Zank;L. Burlaga;R. Decker;E. Stone
通讯作者：
N. Pogorelov;S. Borovikov;G. Zank;L. Burlaga;R. Decker;E. Stone