ASTROPHYSICAL FLUID DYNAMICS

Degree course: 
Corso di Second cycle degree in PHYSICS
Academic year when starting the degree: 
2025/2026
Year: 
1
Academic year in which the course will be held: 
2025/2026
Course type: 
Compulsory subjects, characteristic of the class
Credits: 
6
Period: 
First Semester
Standard lectures hours: 
48
Detail of lecture’s hours: 
Lesson (48 hours)
Requirements: 

Physics and mathematics courses of the bachelor’s degree (in particular mechanics, electromagnetism and basic thermodynamics)

Final Examination: 
Orale

Oral exam divided in two parts. The first part is a presentation on a topic not covered in the course prepared by the student. The second part includes questions on both theory and exercises.

Assessment: 
Voto Finale

Fluid dynamics is one of the most central branches of astrophysics. It is essential to understand the formation of stars, the dynamics of galaxies (what is the origin of spiral structure?), accretion onto central objects (how are black holes fuelled?), supernovae explosions, cosmological flows, the structure of stars, planet atmospheres, the interstellar medium, and the list could go on. The goal of this course is to equip the students with the main theoretical tools to study the dynamics of fluids in astrophysical systems. At the end of the course the student will be able to: - identify the correct set of fluid equations appropriate for modelling a variety of astrophysical system - understand the solutions of several astrophysical classic fluid problems - analytically solve the fluid equations in some simple cases - tackle new problems in the field of astrophysical fluid dynamics

- Fundamentals of hydrodynamics: continuity and Euler equations, equation of state, conservation of mass/momentum/energy, viscosity and thermal conduction, Lagrangian vs Eulerian views, vorticity equation, Kelvin circulation theorem, rotating frames, Reynolds number, radiative heating and cooling. - Fundamentals of magneto-hydrodynamics: MHD equations, induction equation, magnetic pressure and tension, magnetic flux freezing, magnetic fields amplification. - Hydrostatic equilibrium: polytropic and isothermal spheres, polytropic and isothermal slabs, application: Chandrasekhar upper mass limit for white dwarfs - Spherical steady flows: Parker solar wind and Bondi spherical accretion - Waves: sound waves, water waves, group velocity, analogy between shallow water theory and gas dynamics, MHD waves (Alfvén waves. fast and slow waves), internal gravity waves. Effects of rotation on waves, epicyclic frequency and Lindblad resonances, density waves in discs - Shocks: steepening of sound waves and the formation of shocks, 1D jump conditions at discontinuity (Rankine-Hugoniot conditions), Mach number - Spherical blast waves: strong explosion in uniform atmosphere, Sedov-Taylor self-similar solution, application: supernovae - Accretion discs: Eddington limit, basic equations of viscous thin disc evolution, steady-state viscous thin discs, angular momentum transport, Shakura-Sunyaev alpha-disc model, emitted spectrum, vertical and radial balance, time-dependent accretion - Instabilities: Kelvin-Helmholtz instability, Thermal instability, Rayleigh instability, rotational instability and Rayleigh criterion, magneto-rotational instability, Jeans instability, Toomre instability - Gravity: Legendre expansion, Gauss’s Law, Poisson equation, Tidal forces, Virial theorem. Tides, the equilibrium tide, stability of satellites in orbit around the Earth - Elements of turbulence, Kolmogorov’s theory

Frontal teaching on a blackboard. Lecture notes will be provided

For any question, discussion, concern, etc, students are invited to contact the teacher at the following email: mattiacarlo.sormani@uninsubria.it