Large Scale Earth's Bow Shock with Northern IMF as simulated by PIC code in parallel with MHD model

TL;DR

This paper introduces a stable 3D kinetic PIC model for Earth's bow shock, validated against MHD simulations, revealing detailed plasma behaviors and magnetic structures with computational efficiency.

Contribution

The paper presents a new stable, resource-efficient 3D PIC model for Earth's bow shock, validated against MHD, and capable of capturing macrostructures and kinetic effects.

Findings

Earth's bow shock position is ~14.8 RE along Sun-Earth line.

Shock jump conditions are reproduced in both models.

PIC density and temperature are inflated and shifted sunward.

Abstract

In this paper, we propose a 3D kinetic model (Particle-in-Cell PIC ) for the description of the large scale Earth's bow shock. The proposed version is stable and does not require huge or extensive computer resources. Because PIC simulations work with scaled plasma and field parameters, we also propose to validate our code by comparing its results with the available MHD simulations under same scaled Solar wind ( SW ) and ( IMF ) conditions. We report new results from the two models. In both codes the Earth's bow shock position is found to be ~14.8 RE along the Sun-Earth line, and ~ 29 RE on the dusk side. Those findings are consistent with past in situ observations. Both simulations reproduce the theoretical jump conditions at the shock. However, the PIC code density and temperature distributions are inflated and slightly shifted sunward when compared to the MHD results. Kinetic electron motions and reflected ions upstream may cause this sunward shift. Species distributions in the foreshock region are depicted within the transition of the shock (measured ~2 c/{\omega}pi for {\Theta}Bn =90o and MMS =4.7 ) and in the downstream. The size of the foot jump in the magnetic field at the shock is measured to be (1.7 c/{\omega}pi ). In the foreshocked region, the thermal velocity is found equal to 213 km.sec-1 at 15 RE and is equal to 63 km.sec-1at 12 RE (Magnetosheath region). Despite the large cell size of the current version of the PIC code, it is powerful to retain macrostructure of planets magnetospheres in very short time, thus it can be used for a pedagogical test purposes. It is also likely complementary with MHD to deepen our understanding of the large scale magnetosphere