Three‐Dimensional Global Hybrid Simulations of High Latitude Magnetopause Reconnection and Flux Ropes During the Northward IMF

Guo, Jin; Lu, San; Lu, Quanming; Lin, Y.; Wang, Xueyi; Zhang, Qinghe; Zou, Xing; Huang, Kai; Wang, Rongsheng; Wang, Shui

doi:10.1029/2021gl095003

Cited by 11 publications

(11 citation statements)

References 44 publications

(105 reference statements)

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“…These FTEs may coalesce with each other because of their different propagating speeds, and new FTEs are generated at the magnetopause near Mercury. The coalescence of FTEs is a re-reconnection process, which has also been well simulated and studied by performing 3D global hybrid simulations at the Earth's magnetopause (Guo et al 2021a(Guo et al , 2021b(Guo et al , 2021c and ubiquitously observed in planetary magnetospheres (Wang et al 2017;Zhou et al 2017;Zhong et al 2020). At t = 135.72 s, F2 and F3 have merged into one FTE "F2,3," and a new FTE "F4" appears at about x = −0.5R M .…”

Section: Simulation Resultsmentioning

confidence: 96%

Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury

Guo

et al. 2022

ApJ

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One of the important MESSENGER observations is the formation of flux transfer event (FTE) showers, where tens of FTEs are observed in a short time interval of about 1–2 minutes, at Mercury’s magnetopause. In this paper, we investigate the interactions between the solar wind and Mercury’s magnetosphere using three-dimensional global hybrid simulations. When the interplanetary magnetic field (IMF) is purely southward, we can observe FTE showers at the low-latitude dayside magnetopause, and these FTEs can propagate northward or southward with a speed of about 90 km s−1. When the IMF is purely northward, FTE showers can be produced in both the northward and southward hemispheres of the high-latitude nightside magnetopause, and these FTEs propagate toward the magnetotail with a speed of about 250 km s−1. The typical FTEs have a duration of 1–2 s, and reoccur in 5–6 s. Our simulations provide a good explanation for FTE showers observed by MESSENGER.

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Section: Simulation Resultsmentioning

confidence: 96%

Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury

Guo

et al. 2022

ApJ

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“…Based on the above simulation results, Figures 5c and 5d summarize how the IMF

{B}_{y}

controls the azimuthal motion of PMAFs. With

{B}_{y}< 0

, the X‐line of magnetopause reconnection tilts, unparallel to the equatorial plane (Guo et al., 2021a, 2021b, 2021c). Thus, the reconnection outflows (blue arrows in Figure 5c) from the tilted X‐line are dawnward and poleward in the southern hemisphere, and they push the magnetopause flux ropes dawnward and poleward.…”

Section: Resultsmentioning

confidence: 99%

“…In Figure 4a, the flux ropes “1–7” with parallel temperature enhancements are formed by multiple X‐line reconnection in the noon‐midnight meridian plane (Guo et al., 2021b, 2021c; Lee & Fu, 1985; Lee et al., 1993; Tan et al., 2011). These flux ropes are formed at low latitudes and then move to higher latitudes.…”

Section: Resultsmentioning

confidence: 99%

“…The lifetime (∼3 min) of the flux rope is consistent with that of the PMAF (Figure 2b), but the azimuthal velocity of the flux rope is faster than that of PMAF (Figure 2b), which may be due to the faster magnetopause reconnection and outflows caused by the strong IMF in the solar wind. We also perform a simulation with a positive IMF 𝐴𝐴 𝐴𝐴𝑦𝑦 , and in the case, the representative flux rope in the southern hemisphere moves duskward for about 1.58 hr MLT With 𝐴𝐴 𝐴𝐴𝑦𝑦 < 0 , the X-line of magnetopause reconnection tilts, unparallel to the equatorial plane (Guo et al, 2021a(Guo et al, , 2021b(Guo et al, , 2021c. Thus, the reconnection outflows (blue arrows in Figure 5c) from the tilted X-line are dawnward and poleward in the southern hemisphere, and they push the magnetopause flux ropes dawnward and poleward.…”

Section: 1029/2022gl099753mentioning

confidence: 99%

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Azimuthal Motion of Poleward Moving Auroral Forms

Guo

Wang

et al. 2022

Geophysical Research Letters

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Aurora, a colorful and dynamic light display that illuminates Earth's polar regions, is caused by energetic particles precipitating to the ionosphere along magnetic field lines (Jones, 2012). The aurora is not only visually spectacular but also important in science because it monitors various dynamic processes during the interactions between the solar wind and the magnetosphere (Frey et al., 2003;Sandholt & Farrugia, 2003;Southwood, 1987). The interactions are dramatically intensified when the magnetic field in the solar wind, that is, interplanetary magnetic field (IMF), has a southward component and reconnects with the northward geomagnetic field at the dayside magnetopause (Dungey, 1961;Russell & Elphic, 1978). This reconnection process forms flux transfer events (FTEs) or flux ropes that correspond to the most common dayside auroral structure in the ionosphere, poleward moving auroral form (PMAF), which recurs every 5-15 min (

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“…Hybrid codes have been used for modeling large systems such as (small or artificially reduced) planetary magnetospheres. However such large scale models typically poorly resolve the Hall scale [5,6,7,8]. Not resolving such sub-ion scale current sheets may result in errors leading to spurious macroscopic behavior [9].…”

Section: Introductionmentioning

confidence: 99%

Hybrid Particle-In-Cell model with Adaptive Mesh Refinement

Aunai¹,

Smets²,

Deegan³

et al. 2022

Preprint

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Collisionless magentized plasmas a priori need to be evolved using Vlasov-Maxwell kinetic formalism. However the tremendous number of spatial and temporal scales involved in phenomena of interest makes it prohibitive, from a computational standpoint. Fully kinetic particle in cell and single fluid MHD codes are commonly used at very small or very large scales. The hybrid formalism, treating ions kinetically and electrons as a fluid, is in principle advantageous to fill the gap between these two extremities. However, a correct treatment of critical regions such as reconnection X-lines require a good resolution of sub-ion dissipative scales, which still constitute a major challenge if aiming at simulating meso/macro scale systems. This work presents a new code, named PHARE, which successfully implements the adaptive mesh refinement mechanism in a hybrid particle-in-cell code. Such a code is able to dynamically focus the resolution in critical regions while others not only have a coarser spatial resolution, but are also evolved much less often thanks to a recursive time stepping procedure. Adopting a patch based AMR mechanism, the code architecture is made so that the specific solver/physical model that is solved at a given refined level is abstracted, thus giving the opportunity to handling multi-formalisms AMR patch hierarchies, where, for instance, coarsest levels are solved in MHD while dynamicall created refined levels are solved within the Hybrid framework.

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Three‐Dimensional Global Hybrid Simulations of High Latitude Magnetopause Reconnection and Flux Ropes During the Northward IMF

Cited by 11 publications

References 44 publications

Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury

Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury

Azimuthal Motion of Poleward Moving Auroral Forms

Hybrid Particle-In-Cell model with Adaptive Mesh Refinement

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