It is well-known that interplanetary magnetic clouds can cause stronggeomagnetic storms due to the high magnetic field magnitude in theirinterior, especially if there is a large negative Bz component present. Inaddition, the magnetic disturbances around such objects can play an importantrole in their "geo-effectiveness". On the other hand, the magnetic and flowfields in the CME sheath region in front of the body and in the rear of thecloud are important for understanding both the dynamics and the evolution ofthe interplanetary cloud. The "eventual" aim of this work is to calculate themagnetic field in this CME sheath region in order to evaluate the possiblegeo-efficiency of the cloud in terms of the maximum |Bz|-component in thisregion. In this paper we assess the potential of this approach by introducinga model with a simplified geometry. We describe the magnetic field betweenthe CME shock surface and the cloud's boundary by means of a vectorpotential. We also apply our model and present the magnetic fielddistribution in the CME sheath region in front of the body and in the rear ofthe cloud formed after the event of 20 November 2003.
展开▼
机译：众所周知，由于行星际内部的磁场强度高，尤其是存在负的 B z 分量时，行星际磁云会引起强地磁风暴。此外，这些物体周围的磁干扰在其“地球效应”中可能起重要作用。另一方面，机体前方和云后方CME鞘区域中的磁场和流场对于理解行星际云的动力学和演化都很重要。这项工作的“最终”目的是计算此CME护套区域中的磁场，以便根据最大| B z |-在此区域中。在本文中，我们通过引入具有简化几何形状的模型来评估这种方法的潜力。我们通过矢量势描述了CME激波表面和云边界之间的磁场。我们还应用了我们的模型，并介绍了2003年11月20日事件后身体前部CME护套区域和云层后部CME护套区域的磁场分布。
展开▼
