2023
DOI: 10.1029/2022ja031068
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Kinetic Simulation of Cold Ion Heating in Asymmetric Reconnection

Abstract: Cold ions from the plasmasphere can reach the Earth's magnetopause through the plasma wind and plume, affecting the reconnection at the magnetopause, such as changing the reconnection rate and influencing the energy budget. Recent observations found that cold ions were substantially heated by magnetopause reconnection. Although a few mechanisms have been proposed to account for the cold ion acceleration at the magnetopause, the dominant mechanism remains unclear. In this paper, we perform 2.5‐dimensional fully… Show more

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“…In our simulation, we observe that the dimensionless reconnection rate peaks with E r ∼ 0.09 at t ≈ 18 and becomes quasi‐steady after t ≈ 30 with E r ∼ 0.07 (Song et al., 2023a). However, at t ≈ 55, the reconnection rate begins to decline due to the saturation of the tearing mode caused by the ideal conducting boundary condition.…”
Section: Simulation Resultsmentioning
confidence: 59%
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“…In our simulation, we observe that the dimensionless reconnection rate peaks with E r ∼ 0.09 at t ≈ 18 and becomes quasi‐steady after t ≈ 30 with E r ∼ 0.07 (Song et al., 2023a). However, at t ≈ 55, the reconnection rate begins to decline due to the saturation of the tearing mode caused by the ideal conducting boundary condition.…”
Section: Simulation Resultsmentioning
confidence: 59%
“…As depicted in Figures 1a and 1b, a robust electric field E z is present at the magnetospheric separatrix region ( z ∼ −1) throughout the reconnection, pointing from the magnetosphere to the magnetosheath ( E z > 0). Previous simulations of asymmetric reconnection have revealed the presence of this electric field (Burch et al., 2016; Dargent et al., 2019; Malakit et al., 2013; Shay et al., 2016; Wang et al., 2017), which is balanced by the Hall term in generalized Ohm's law (Malakit et al., 2013; Song et al., 2023a), indicating that it is a Hall electric field. The magnitude of the Hall electric field E z at t = 50 (Figure 1b) is smaller than that at t = 30 (Figure 1a) and is weaker in the vicinity of the X‐line than in the magnetospheric separatrix region (Figures 1a and 1b).…”
Section: Simulation Resultsmentioning
confidence: 93%
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