Space plasma environment of Mars

Mars, unlike Earth, lacks a global magnetic field that would shield it from the direct influence of the solar wind. Instead, the solar wind induces currents in the ionosphere, forming what is known as an induced magnetosphere. A magnetic pile-up boundary can be identified, along with a bow shock farther upstream due to the supersonic nature of the solar wind. The interaction is further complicated by the presence of remnant crustal magnetic fields, which locally influence the interaction and the ionospheric conditions. As a result, Mars exhibits a highly variable plasma environment governed by numerous factors, fostering irregularities and wave phenomena.

The aim of the thesis is to use plasma and wave measurements from recent spacecraft missions (Mars Express, MAVEN) to investigate the variability of the Martian ionosphere and its interaction with the solar wind. Particular attention is given to wave phenomena, especially in regions of crustal magnetic fields. The study involves both systematic analyses of all available data and case studies of specific events and their effects on the Martian plasma environment. Modern data processing methods, including the potential use of machine learning algorithms, are envisaged to be employed throughout the thesis.

Literature

1. D. A. Gurnett, A. Bhattacharjee: Introduction to Plasma Physics: With Space, Laboratory and Astrophysical Applications. Cambridge University Press, 2005.
2. M. G. Kivelson, C. T. Russell: Introduction to Space Physics. University Press, Cambridge, 1995.
3. G. K. Parks: Physics of Space Plasmas: An Introduction. 2nd ed. Westview Press, 2004.
4. Papers in scientific journals recommended by the thesis supervisor.