10.35099/AURORA-421
Guo, Zhifang
Lin, Yu
Wang, X
Global Hybrid Simulations of Interaction Between Interplanetary Rotational Discontinuity and Bow Shock/Magnetosphere: Can Ion-Scale Magnetic Reconnection be Driven by Rotational Discontinuity Downstream of Quasi-Parallel Shock?
Auburn University
2021
Auburn University
Auburn University
Zhifang Guo, guozf@mail.iggcas.ac.cn
2022-09-29
2022-09-29
2021
Journal Article, Academic Journal
https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2020JA028853?casa_token=hX2L2i33DqYAAAAA%3AZDCOyoeSV8NPhSqT6InzDMaX45sG8A3vP586u5nauRTf7EZTbn2WKrK2w_1aXEQQiARoaMCqS1Bufw
https://aurora.auburn.edu/handle/11200/50353
PDF
©American Geophysical Union 2021. This is this the version of record co-published by the American Geophysical Union and John Wiley & Sons, Inc. It is made available under the CC-BY-NC-ND 4.0 license. Item should be cited as: Guo, Zhifang, Yu Lin, and Xueyi Wang. "Global Hybrid Simulations of Interaction Between Interplanetary Rotational Discontinuity and Bow Shock/Magnetosphere: Can Ion‐Scale Magnetic Reconnection be Driven by Rotational Discontinuity Downstream of Quasi‐Parallel Shock?." Journal of Geophysical Research: Space Physics 126.4 (2021): e2020JA028853.
Ion-scale magnetic reconnection has been observed downstream of the terrestrial quasi-parallel (Q-parallel to) shock. Whether it is driven by interplanetary discontinuities or turbulent Q-parallel to shock, however, is unclear. Using three-dimensional global hybrid simulation, we investigate the generation of magnetic reconnection downstream of the Q-parallel to shock, while an interplanetary rotational discontinuity (RD) is launched to the bow shock. Cases with various solar wind Alfven Mach numbers, M-A = 3.0 to 8, and propagation directions of the RD are presented. The propagation direction n is assumed to be in the GSE xz plane and pointing earthward, with n = (-sin(theta(12)/2),0,-cos(theta(12)/2)), where theta(12) is the angle between the upstream (B-1) and downstream (B-2) magnetic fields across the transmitted RD. It is found that magnetic reconnection occurs inside the RD downstream of the Q-parallel to shock, forming flux ropes extending along the dawn-dusk direction about tens of ion inertial lengths. Large-amplitude low-frequency waves originated from the Q-parallel to shock lead to the bending and squeezing of the field lines around the RD, which play an important role in triggering reconnection inside the RD. As the RD impacts the dayside magnetopause, magnetopause reconnection takes place between the field lines behind the RD and geomagnetic field lines. Nevertheless, no reconnection is found downstream of the Q-parallel to shock itself or outside the RD in the magnetosheath. The existent and structure of reconnection in the magnetosheath are found to strongly depend on the parameters M-A and n. Our simulation shows that ion-scale magnetic reconnection is driven by an external driver in the form of the compression of an RD around the bow shock and in the magnetosheath, rather than caused by the turbulent Q-parallel to shock alone.