Preprints
https://doi.org/10.5194/angeo-2021-1
https://doi.org/10.5194/angeo-2021-1

  08 Jan 2021

08 Jan 2021

Review status: a revised version of this preprint is currently under review for the journal ANGEO.

Magnetosheath plasma flow model around Mercury

Daniel Schmid, Ferdinand Plaschke, Yasuhito Narita, Martin Volwerk, Rumi Nakamura, and Wolfgang Baumjohann Daniel Schmid et al.
  • Space Research Institute, Austrian Academy of Sciences, Graz, Austria

Abstract. The magnetosheath is defined as the plasma region between the bow shock, where the super-magnetosonic solar wind plasma is decelerated and heated, and the outer boundary of the intrinsic planetary magnetic field, the so called magnetopause. Based on the Soucek-Escoubet magnetosheath flow model at Earth, we present the first analytical magnetosheath plasma flow model for Mercury. It can be used to estimate the plasma flow magnitude and direction at any given point in the magnetosheath exclusively on the basis of the plasma parameters of the upstream solar wind. The aim of this paper is to provide a tool to back-trace the magnetosheath plasma flow between multiple observation points or from a given spacecraft location to the bow shock.

Daniel Schmid et al.

Status: final response (author comments only)

Comment types: AC – author | RC – referee | CC – community | EC – editor | CEC – chief editor | : Report abuse
  • RC1: 'Comment on angeo-2021-1', Anonymous Referee #1, 26 Jan 2021
  • RC2: 'Comment on angeo-2021-1', Anonymous Referee #2, 03 Feb 2021

Daniel Schmid et al.

Daniel Schmid et al.

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Short summary
In this work we present the first analytical magnetosheath plasma flow model for the space environment around Mercury. The proposed model is relatively simple to implement and provides the possibility to trace the flowlines inside the Hermean magnetosheath. It can help to determine the the local plasma conditions of a spacecraft in the magnetosheath exclusively on basis of the upstream solar wind parameters.