Student: Abushzada Ilyas
Školitel: Mgr. Alexander Pitňa, Ph.D.
Konzultant: Prof. RNDr. Jana Šafránková, DrSc.
Stav práce: zadaná
Anotace:
The solar wind, a continuous stream of charged particles emanating from the Sun's corona, serves as a medium for studying magnetohydrodynamic (MHD) turbulence. Turbulent processes play a key role in the dynamics of solar wind plasma fluctuations, governing energy transfer within the heliosphere that leads to particle acceleration.
On scales larger than the characteristic ion scales, proton inertial length and proton thermal gyroradius, solar wind plasma can be well described by equations of magnetohydrodynamics, nevertheless, the nature of the fluctuations at these scales is still debated.
We aim to investigate the nature of the large and small scale fluctuations in the turbulent solar wind, with a focus on elucidating the fundamental processes governing energy transport and plasma dynamics in the heliosphere. By investigating the magnetic field fluctuations in the framework of traditional and recently developed methods, we suppose to study the role of various modes (Alfvénic, fast and slow) and their evolution throughout the heliosphere. A comprehensive approach integrating observational analysis (using a fleet of spacecraft operating in different distances from the Sun) and theoretical modeling (based on the Zank theory [2023]) will contribute to our understanding of solar wind dynamics.
Literature
Russell, C.T., Luhmann, J.G. and Strangeway, R.J. (2016) Space Physics: An Introduction. Cambridge: Cambridge University Press.
Glassmeier, K.H. et al. (1995) Mode recognition of MHD wave fields at incomplete dispersion measurements. Annales Geophysicae, vol. 13, no. 1, p. 76-83
Zank, G.P. (2014) Transport Processes in Space Physics and Astrophysics. Springer
Zank, G.P. (2023) Linear Mode Decomposition in Magnetohydrodynamics Revisited, The Astrophysical Journal Supplement Series, 268:18 (38pp)