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Last update: T_AUUK (26.03.2015)
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Last update: prof. RNDr. David Vokrouhlický, DrSc. (10.06.2019)
Oral examination. |
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Last update: RNDr. Miroslav Bárta, Ph.D. (09.02.2024)
Karlický, M. (2015): Plasma Astrophysics, Mafyzpress, ISBN 9788073782818
Priest, E.R. (2000): Solar magnetohydrodynamics, D. Reidel Publishing
Kulsrud, R.M. (2005): Plasma physics for astrophysics, Princeton University Press
Aschwanden M.(2006): Physics of the solar corona, Springer
Biskasmp, D. (2000): Magnetic reconnection in plasmas, Cambridge University Press
Biskamp, D. (2003): Magnetohydrodynamic turbulence, Cambridge University Press
Stix, M.(1989): The Sun. An Introduction, Springer-Verlag
Press, W.H., Teukolsky, S.A., Vetterling, W.T., Flannery, B.P. (1992): Numerical Recipes in FORTRAN and C, Part I and II, Cambridge Univeristy Press
Chung, T.J. (2006): Computational Fluid Dynamics, Cambridge University Press
Versteeg H.K., Malasekera W. : An introduction to computational fluid dynamics - The finite volume methods, Pearson/Prentice Hall 2007
Birdsall, C.K., Langdon, A.B. (2004): Plasma Physics Via Computer Simulation, Taylor & Francis Ltd.
On-line resources:
Living Reviews in Solar Physics
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Last update: RNDr. Miroslav Bárta, Ph.D. (09.02.2024)
Lecture series finished by a hands-on session with illustrative simple examples of numerical modelling in the astrophysics of the solar atmosphere. Excursion to observatory of the Astronomical Institute of the Czech Academy of Sciences in Ondrejov. |
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Last update: prof. RNDr. David Vokrouhlický, DrSc. (14.01.2019)
Basic consents of plasma physics and their application to processes in the solar atmosphere. Kinetic, two-fluid and MHD description of plasmas: (single-)fluid model as an approximation and limits of its usability. Generalized Ohm’s law and anomalous (effective) electrical resistivity. Coupling of macro- and micro-scales in solar plasmas.
Macroscopic structures of magnetic field in the solar atmosphere: Loops, flux ropes, and arcades. Magnetic field extrapolations: linear and non-linear force-free fields. Basics of solar magneto-hydrostatics (MHS): Example calculations of MHS equilibria - prominences/filaments, vertical slabs and tubes. Magneto/hydrodynamic waves in wave-guides: Classification of the wave-modes, MHS structures in the solar atmosphere as wave-guides, applications - coronal seismology.
Magnetic-field topology and its changes. Topological skeleton of the magnetic field: Null points, separators, separatrix surfaces and quasi-separatrix layers (QSLs). Helicity. Topological changes of the magnetic field - magnetic field-line reconnection.
Magnetic reconnection - deeper look: current-layer (in)stability (tearing mode), classical reconnection models (Sweet-Parker, Petchek) and their limitations, non-linear stage of the tearing-mode instability - formation of magnetic islands/plasmoids. Plasmoid instability in highly-conductive plasmas. Dimensionality aspects: 2D vs. 3D reconnection. Magnetic configurations prone to formation of the current concentrations (current sheets): Null points, separators, (quasi)separatrix layers. (Turbulent) Energy cascades in the magnetic reconnection. Different reconnection regimes - parametric “phase diagram” of reconnection.
Occurrence and meaning of magnetic reconnection in the solar and astrophysical plasmas. Application of the MHD-instabilities theory and reconnection physics in solar research: Solar eruptive flares and CMEs.
Modeling of macroscopic processes in plasmas. Structure of the MHD equations: Energetics of the MHD processes and MHD equations in the conservative form. Approximative solution of the Riemann problem in MHD. Basic approaches to the numerical MHD modeling: Finite differences (FDM), volumes (FVM), and elements (FEM) methods of discretisation. Introduction to advanced techniques: Adaptive Mesh Refinement (AMR), parallelisation (MPI, CUDA) of numerical algorithms and high-performance computing (HPC). Micro-scale kinetic processes in plasmas. Cascading energy transfer towards micro-scales and MHD turbulence. Particle acceleration, formation of non-Maxwellian distribution functions. Plasma micro-instabilities: Plasma+particle-beam systems and other non-Maxwellian configurations, generation of high-frequency plasma waves.
Analytical description of driven/damped waves in plasmas - quasi-linear (QL) approximation. Generalized plasma dielectric tensor. Kinetic equations for QL approximation. Energetics in the waves, absorption and emission coefficients. Stimulated emission vs. Landau damping. Feedback of plasma micro-physics to (effective) transport coefficients (e.g. resistivity) - scale coupling.
Numerical approaches to modeling of small-scale (kinetic) processes in the solar plasmas: Particle codes - Test particle (TP) and Particle-in-Cell (PIC), Vlasov simulations, gyro-kinetic approximation.
Modern multi-wavelength observations as a remote diagnostics of solar plasmas and test of our models. Relations between model and observation - forward fitting and inversion methods. Significance of the diagnostic layer above numerical models - calculation of observables from the state variables of the simulated system. Numerical simulations with observation-driven boundary conditions. Cascade of consecutive simulations for the space weather predictions - CACTUS. |
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Last update: RNDr. Miroslav Bárta, Ph.D. (09.02.2024)
The course is running in the even years only (beginnings in October 2024, 2026, 2028,...)!
Prerequisites: Solar physics I, Plasma physics / Space electrodynamics. |