26 Jul 2022
26 Jul 2022
Status: this preprint is open for discussion.

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

Cyril Simon Wedlund1, Martin Volwerk1, Christian Mazelle2, Sebastián Rojas Mata3, Gabriella Stenberg Wieser3, Yoshifumi Futaana3, Jasper Halekas4, Diana Rojas-Castillo5, César Bertucci6, and Jared Espley7 Cyril Simon Wedlund et al.
  • 1Austrian Academy of Sciences, Space Research Institute, Graz, Austria
  • 2Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
  • 3Swedish Institute of Space Physics, Kiruna, Sweden
  • 4Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA
  • 5Instituto de Geofísica, Universidad Nacional Autónoma de México, Coyoacán, Mexico
  • 6Instituto de Astronomía y Física del Espacio, Ciudad Autónoma de Buenos Aires, Argentina
  • 7NASA Goddard Space Flight Center, Laboratory for Planetary Magnetospheres, Greenbelt, MD, USA

Abstract. In this series of papers, we present statistical maps of mirror mode-like (MM) structures in the magnetosheaths of Mars and Venus and calculate the probability of detecting them in spacecraft data. We aim to study and compare them with the same tools and a similar payload at both planets. We consider their dependence on Extreme Ultraviolet (EUV) solar flux levels (high and low), and, specific to Mars, on Mars Year (MY) as well as atmospheric seasons (four solar longitudes Ls). We first use magnetic field-only criteria to detect these structures and present ways to mitigate ambiguities in the nature of the detected structures. In line with many previous studies at Earth, this technique has the advantage of using one instrument (a magnetometer) with good time resolution facilitating comparisons between planetary and cometary environments. Applied to the magnetometer data of the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft from November 2014 to February 2020 (MY32–MY35), we detect structures closely resembling MMs lasting in total more than 170,000 s, corresponding to about 0.1 % of MAVEN's total time spent in the Martian plasma environment. We calculate MM-like occurrences normalised to the spacecraft's residence time during the course of the mission. Detection probabilities are about 1 % at most for any given controlling parameter. In general, MM-like structures appear in two main regions, one behind the shock, the other close to the induced magnetospheric boundary, as expected from theory. Detection probabilities are higher on average in low solar EUV conditions, whereas high solar EUV conditions see an increase in detections within the magnetospheric tail. We tentatively link the former tendency to two combining effects: the favouring of ion cyclotron waves the closer to perihelion due to plasma beta effects, and, possibly, the nongyrotropy of pickup ion distributions. This study is the first of two on the magnetosheaths of Mars and Venus.

Cyril Simon Wedlund et al.

Status: open (until 24 Dec 2022)

Comment types: AC – author | RC – referee | CC – community | EC – editor | CEC – chief editor | : Report abuse

Cyril Simon Wedlund et al.

Cyril Simon Wedlund et al.


Total article views: 251 (including HTML, PDF, and XML)
HTML PDF XML Total BibTeX EndNote
193 51 7 251 2 3
  • HTML: 193
  • PDF: 51
  • XML: 7
  • Total: 251
  • BibTeX: 2
  • EndNote: 3
Views and downloads (calculated since 26 Jul 2022)
Cumulative views and downloads (calculated since 26 Jul 2022)

Viewed (geographical distribution)

Total article views: 228 (including HTML, PDF, and XML) Thereof 228 with geography defined and 0 with unknown origin.
Country # Views %
  • 1
Latest update: 29 Nov 2022
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, the other closer to the planet. They compete with other wave modes depending on the solar flux and heliocentric distance.