Articles | Volume 41, issue 1
Regular paper
31 May 2023
Regular paper |  | 31 May 2023

Statistical distribution of mirror-mode-like structures in the magnetosheaths of unmagnetised planets – Part 1: Mars as observed by the MAVEN spacecraft

Cyril Simon Wedlund, Martin Volwerk, Christian Mazelle, Sebastián Rojas Mata, Gabriella Stenberg Wieser, Yoshifumi Futaana, Jasper Halekas, Diana Rojas-Castillo, César Bertucci, and Jared Espley


Interactive discussion

Status: closed

Comment types: AC – author | RC – referee | CC – community | EC – editor | CEC – chief editor | : Report abuse
  • RC1: 'Comment on egusphere-2022-634', Anonymous Referee #1, 30 Aug 2022
    • AC1: 'Reply on RC1', Cyril Simon Wedlund, 05 Feb 2023
      • AC3: 'Reply on AC1', Cyril Simon Wedlund, 05 Feb 2023
  • RC2: 'Comment on egusphere-2022-634', Anonymous Referee #2, 28 Dec 2022
    • AC2: 'Reply on RC2', Cyril Simon Wedlund, 05 Feb 2023
  • AC4: 'Comment on egusphere-2022-634', Cyril Simon Wedlund, 03 Mar 2023

Peer review completion

AR: Author's response | RR: Referee report | ED: Editor decision | EF: Editorial file upload
ED: Publish subject to revisions (further review by editor and referees) (24 Feb 2023) by Dalia Buresova
AR by Cyril Simon Wedlund on behalf of the Authors (03 Mar 2023)  Author's response   Author's tracked changes   Manuscript 
ED: Referee Nomination & Report Request started (10 Mar 2023) by Dalia Buresova
RR by Anonymous Referee #2 (04 Apr 2023)
ED: Publish as is (21 Apr 2023) by Dalia Buresova
AR by Cyril Simon Wedlund on behalf of the Authors (23 Apr 2023)  Manuscript 
Short summary
Mirror modes are magnetic bottles found in the space plasma environment of planets contributing to the energy exchange with the solar wind. We use magnetic field measurements from the NASA Mars Atmosphere and Volatile EvolutioN mission to detect them around Mars and show how they evolve in time and space. The structures concentrate in two regions: one behind the bow shock and the other closer to the planet. They compete with other wave modes depending on the solar flux and heliocentric distance.