Time‐Dependent Hybrid Plasma Simulations of Lunar Electromagnetic Induction in the Solar Wind

Haviland, H. Fuqua; Poppe, A. R.; Fatemi, Shahab; Delory, G. T.; Pater, Imke de

doi:10.1029/2018gl080523

Cited by 17 publications

(17 citation statements)

References 55 publications

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“…As explained in detail in Fatemi et al (2017), electric fields are directly calculated in the model from the electron momentum equation for massless electrons (i.e., m e = 0), magnetic fields are computed from Faraday's law, and the divergence-free condition of the magnetic field is satisfied over the entire simulation domain. Amitis allows the definition Journal of Geophysical Research: Space Physics 10.1029/2019JA027706 of custom electrical conductivity profiles for the interior of a body from a highly resistive to highly conductive interior with the possibility of defining multiple conductivity layers with and without longitudinal and latitudinal inhomogeneities (Fatemi et al, 2017;Fuqua Haviland et al, 2019). The model self-consistently couples the interior magnetic response to the ambient plasma environment using a semi-implicit method (model details are extensively explained in Fatemi et al, 2017).…”

Section: Modelmentioning

confidence: 99%

“…The model self-consistently couples the interior magnetic response to the ambient plasma environment using a semi-implicit method (model details are extensively explained in Fatemi et al, 2017). Amitis has been previously used to study the plasma interaction with the Moon (Fatemi et al, 2017;Fuqua Haviland et al, 2019;Garrick-Bethell et al, 2019;Poppe, 2019), asteroid 16 Psyche , and Mercury and our simulation results have been previously validated through comparison with analytical theories (Fuqua Haviland et al, 2019) and with ARTEMIS and MESSENGER observations (Fatemi et al, 2017Poppe, 2019).…”

Section: Modelmentioning

confidence: 99%

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Hybrid Simulations of Solar Wind Proton Precipitation to the Surface of Mercury

2020

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We examine the effects of the interplanetary magnetic field (IMF) orientation and solar wind dynamic pressure on the solar wind proton precipitation to the surface of Mercury using a hybrid-kinetic model. We use our model to explain observations of Mercury's neutral sodium exosphere and compare our results with MESSENGER observations. For the typical solar wind dynamic pressure at Mercury our model shows a high proton flux precipitates through the magnetospheric cusps to the high latitudes on both hemispheres on the dayside, centered near the noon meridian with ∼11 • latitudinal extent in the north and ∼21 • latitudinal extent in the south, which is consistent with MESSENGER observations. We show that this two-peak pattern is controlled by the radial component (B x ) of the IMF and not the B z . Our model suggests that the southward IMF and its associated magnetic reconnection do not play a major role in controlling plasma precipitation to the surface of Mercury through the cusps. We found that the total precipitation rate through both of the cusps remain constant and independent of the IMF orientation. We also show that the solar wind proton incidence rate to the entire surface of Mercury is higher when the IMF has a northward component and nearly half of the incidence flux impacts the low latitudes on the nightside. During extreme solar events (e.g., coronal mass ejections), our model suggests that over 70 nPa solar wind dynamic pressure is required for the entire surface of Mercury to be exposed to the solar wind plasma.

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Section: Modelmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

Hybrid Simulations of Solar Wind Proton Precipitation to the Surface of Mercury

2020

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“…This allows the hybrid model to provide a more accurate description of the ion physics at this scale while not being as computationally expensive as a purely kinetic model. Numerous studies have used Amitis to model solar wind interactions with planetary bodies ranging in size from asteroids to Mercury (Fatemi et al, 2017Fatemi & Poppe, 2018Fuqua Haviland et al, 2019;Garrick-Bethell et al, 2019;. Amitis runs were performed assuming a lunar conductivity of 10 −7 S/m and using two different sets of time-dependent upstream boundary conditions, each running until a steady-state is obtained.…”

Section: Hybrid Model and Setupmentioning

confidence: 99%

“…This allows the hybrid model to provide a more accurate description of the ion physics at this scale while not being as computationally expensive as a purely kinetic model. Numerous studies have used Amitis to model solar wind interactions with planetary bodies ranging in size from asteroids to Mercury (Fatemi et al., 2017, 2018, 2020 Fatemi & Poppe, 2018; Fuqua Haviland et al., 2019; Garrick‐Bethell et al., 2019; Poppe, 2019).…”

Section: The Anomalous Appearance Of a Lunar Wake At Full Moonmentioning

confidence: 99%

A Double Disturbed Lunar Plasma Wake

et al. 2021

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Under nominal solar wind conditions, a tenuous wake forms downstream of the lunar nightside. However, the lunar plasma environment undergoes a transformation as the Moon passes through the Earth's magnetotail, with hot subsonic plasma causing the wake structure to disappear. We investigate the lunar wake response during a passing coronal mass ejection (CME) on March 8, 2012 while crossing the Earth's magnetotail using both a magnetohydrodynamic (MHD) model of the terrestrial magnetosphere and a three‐dimensional hybrid plasma model of the lunar wake. The CME arrives at 1 AU around 10:30 UT and its impact is first detected inside the geomagnetic tail after 11:10 UT by the Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun (THEMIS‐ARTEMIS) satellites in lunar orbit. A global magnetospheric MHD simulation using Wind data for upstream conditions with the OpenGGCM model reveals the magnetosheath compression to the lunar position from 11:20–12:00 UT, accompanied by multiple flux rope or plasmoid‐like features developing and propagating tailward. MHD results support plasma changes observed by the THEMIS‐ARTEMIS satellites. Lunar‐scale simulations using the Amitis hybrid code show a short and misaligned plasma wake during the Moon's brief entry into the magnetosheath at 11:20 UT, with plasma expansion into the void being aided by the higher plasma temperatures. Sharply accelerated flow speed and a compressed magnetic field lead to an enhanced electric field in the lunar wake capable of generating sudden changes to the nightside near‐surface electric potential.

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“…Thus, this model is ideal for examining the solar wind plasma interaction with the Moon and for the formation of the trailing wake region that extends many lunar radii downstream. Numerous studies have used Amitis to model solar wind interactions with planetary bodies ranging in size from asteroids to Mercury (Fatemi et al 2017(Fatemi et al , 2020Fatemi & Poppe 2018;Fuqua Haviland et al 2019;Garrick-Bethell et al 2019;Poppe 2019;Rasca et al 2021).…”

Section: Modelmentioning

confidence: 99%

Modeling the Lunar Wake Response to a CME Using a Hybrid PIC Model

Rasca¹,

Fatemi²,

Farrell³

2022

Planet. Sci. J.

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In the solar wind, a low-density wake region forms downstream of the nightside lunar surface. In this study, we use a series of 3D hybrid particle-in-cell simulations to model the response of the lunar wake to a passing coronal mass ejection (CME). Average plasma parameters are derived from the Wind spacecraft located at 1 au during three distinct phases of a passing halo (Earth-directed) CME on 2015 June 22. Each set of plasma parameters, representing the shock/plasma sheath, a magnetic cloud, and plasma conditions we call the mid-CME phase, are used as the time-static upstream boundary conditions for three separate simulations. These simulation results are then compared with results that use nominal solar wind conditions. Results show a shortened plasma void compared to nominal conditions and a distinctive rarefaction cone originating from the terminator during the CME’s plasma sheath phase, while a highly elongated plasma void reforms during the magnetic cloud and mid-CME phases. Developments of electric and magnetic field intensification are also observed during the plasma sheath phase along the central wake, while electrostatic turbulence dominates along the plasma void boundaries and 2–3 lunar radii R M downstream in the central wake during the magnetic cloud and mid-CME phases. The simulations demonstrate that the lunar wake responds in a dynamic way with the changes in the upstream solar wind during a CME.

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Time‐Dependent Hybrid Plasma Simulations of Lunar Electromagnetic Induction in the Solar Wind

Cited by 17 publications

References 55 publications

Hybrid Simulations of Solar Wind Proton Precipitation to the Surface of Mercury

Hybrid Simulations of Solar Wind Proton Precipitation to the Surface of Mercury

A Double Disturbed Lunar Plasma Wake

Modeling the Lunar Wake Response to a CME Using a Hybrid PIC Model

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