Subscribe to the gold package and get unlimited access to Shamra Academy
Register a new userElectron Physics in 3D Two-Fluid Ten-Moment Modeling of Ganymedes Magnetosphere
239
0
0.0
(
0
)
Ask ChatGPT about the research
No Arabic abstract
We studied the role of electron physics in 3D two-fluid 10-moment simulation of the Ganymedes magnetosphere. The model captures non-ideal physics like the Hall effect, the electron inertia, and anisotropic, non-gyrotropic pressure effects. A series of analyses were carried out: 1) The resulting magnetic field topology and electron and ion convection patterns were investigated. The magnetic fields were shown to agree reasonably well with in-situ measurements by the Galileo satellite. 2) The physics of collisionless magnetic reconnection were carefully examined in terms of the current sheet formation and decomposition of generalized Ohms law. The importance of pressure anisotropy and non-gyrotropy in supporting the reconnection electric field is confirmed. 3) We compared surface brightness morphology, represented by surface electron and ion pressure contours, with oxygen emission observed by the Hubble Space Telescope (HST). The correlation between the observed emission morphology and spatial variability in electron/ion pressure was demonstrated. Potential extension to multi-ion species in the context of Ganymede and other magnetospheric systems is also discussed.
rate research
Read More
In a cross-field (ExB) setup, the electron ExB flow relative to the unmagnetized ions can cause the Electron Cyclotron Drift Instability (ECDI) due to resonances of the ion-acoustic mode and the electron cyclotron harmonics. This occurs in collisionless shocks in magnetospheres and in ExB discharge devices such as Hall thrusters. ECDI induces an electron flow parallel to the background E field at a speed greatly exceeding predictions by classical collision theory. Such anomalous transport might cause unfavorable plasma flows towards the walls of ExB devices. Prediction of ECDI and anomalous transport is often thought to require a fully kinetic treatment. In this work, however, we demonstrate that a reduced variant of this instability, and more importantly, the anomalous transport, can be treated self-consistently in a collisionless two-fluid framework without any adjustable collision parameter, by treating both electron and ion species on an equal footing. We will first present linear analyses of the instability in the two-fluid 5- and 10-moment models, and compare them against the fully kinetic theory. At low temperatures, the two-fluid models predict the fastest-growing mode comparable to the kinetic results. Also, by including more moments, secondary (and possibly higher) unstable branches can be recovered. The dependence of the instability on ion-to-electron mass ratio, plasma temperature, and the background field strength is also thoroughly explored. We then carry out 5-moment simulations of the cross-field setup. The development of the instability and the anomalous transport are confirmed and in excellent agreement with theoretical predictions. The force balance properties are also studied. This work casts new insights into the nature of ECDI and the induced anomalous transport and demonstrates the potential of the two-fluid moment model in the efficient modeling of ExB plasmas.
For the first time, we explore the tightly coupled interior-magnetosphere system of Mercury by employing a three-dimensional ten-moment multifluid model. This novel fluid model incorporates the non-ideal effects including the Hall effect, inertia, and tensorial pressures that are critical for collisionless magnetic reconnection; therefore, it is particularly well suited for investigating $collisionless$ magnetic reconnection in Mercurys magnetotail and at the planets magnetopause. The model is able to reproduce the observed magnetic field vectors, field-aligned currents, and cross-tail current sheet asymmetry (beyond the MHD approach) and the simulation results are in good agreement with spacecraft observations. We also study the magnetospheric response of Mercury to a hypothetical extreme event with an enhanced solar wind dynamic pressure, which demonstrates the significance of induction effects resulting from the electromagnetically-coupled interior. More interestingly, plasmoids (or flux ropes) are formed in Mercurys magnetotail during the event, indicating the highly dynamic nature of Mercurys magnetosphere.
The moment-of-fluid method (MOF) is an extension of the volume-of-fluid method with piecewise linear interface construction (VOF-PLIC). In MOF reconstruction, the optimized normal vector is determined from the reference centroid and the volume fraction by iteration. The state-of-art work by citet{milcent_moment--fluid_2020} proposed an analytic gradient of the objective function, which greatly reduces the computational cost. In this study, we further accelerate the MOF reconstruction algorithm by using Gauss-Newton iteration instead of Broyden-Fletcher-Goldfarb-Shanno (BFGS) iteration. We also propose an improved initial guess for MOF reconstruction, which improves the efficiency and the robustness of the MOF reconstruction algorithm. Our implementation of the code and test cases are available on our Github repository.
Using measurements from the Cassini spacecraft in Saturns magnetosphere, we propose a 3D physical picture of a corotating reconnection site, which can only be driven by an internally generated source. Our results demonstrate that the corotating magnetic reconnection can drive an expansion of the current sheet in Saturns magnetosphere and, consequently, can produce Fermi acceleration of electrons. This reconnection site lasted for longer than one of Saturns rotation period. The long-lasting and corotating natures of the magnetic reconnection site at Saturn suggest fundamentally different roles of magnetic reconnection in driving magnetospheric dynamics (e.g., the auroral precipitation) from the Earth. Our corotating reconnection picture could also potentially shed light on the fast rotating magnetized plasma environments in the solar system and beyond.
The nonlinear evolution of collisionless plasmas is typically a multi-scale process where the energy is injected at large, fluid scales and dissipated at small, kinetic scales. Accurately modelling the global evolution requires to take into account the main micro-scale physical processes of interest. This is why comparison of different plasma models is today an imperative task aiming at understanding cross-scale processes in plasmas. We report here the first comparative study of the evolution of a magnetized shear flow, through a variety of different plasma models by using magnetohydrodynamic, Hall-MHD, two-fluid, hybrid kinetic and full kinetic codes. Kinetic relaxation effects are discussed to emphasize the need for kinetic equilibriums to study the dynamics of collisionless plasmas in non trivial configurations. Discrepancies between models are studied both in the linear and in the nonlinear regime of the magnetized Kelvin-Helmholtz instability, to highlight the effects of small scale processes on the nonlinear evolution of collisionless plasmas. We illustrate how the evolution of a magnetized shear flow depends on the relative orientation of the fluid vorticity with respect to the magnetic field direction during the linear evolution when kinetic effects are taken into account. Even if we found that small scale processes differ between the different models, we show that the feedback from small, kinetic scales to large, fluid scales is negligable in the nonlinear regime. This study show that the kinetic modeling validates the use of a fluid approach at large scales, which encourages the development and use of fluid codes to study the nonlinear evolution of magnetized fluid flows, even in the colisionless regime.
Log in to be able to interact and post comments
comments
Fetching comments
Sign in to be able to follow your search criteria
