. "Astrophysics"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Galactic dynamics"@en . . "5" . "LEARNING OUTCOMES\nThe student will be able to calculate the relaxation and dynamical timescales for galaxies. The student will be able to calculate the gravitational potential for spherical\nand flattened systems. The student will understand the basic principles of direct summation codes, tree codes and particle-mesh codes used to perform numerical\ngalaxy formation simulations. The student will be able to describe the orbits of stars in spherical, axisymmetric and simple non-axisymmetric potentials. The student will be able to use basic integrators. The student will understand how the Boltzmann and Jeans equations can be used in galaxy dynamics. The student will be able to derive the tensor virial theorem. The study will be able to understand the stability of collisionless systems. The student will\nunderstand the basics of relaxation processes in galaxies and understand the thermodynamics of self-gravitating systems. The student will be able to derive the formula\nfor dynamical friction and understand its application. The student will understand the importance of galaxy mergers for galaxy evolution.\n\nCONTENT\nGalactic dynamics is an integral part of modern theoretical astrophysics. The course follows the outline of the second edition of the classic text \"Galactic Dynamics\" by Binney & Tremaine (2008). We begin with a general introduction to galactic dynamics followed by a discussion of relaxation and dynamical timescales. After this we discuss potential theory, how to compute the gravitational potential of galaxies and how to describe galaxies using spherical and flattened density distributions. This is followed by a discussion of Poisson solvers. Then orbit theory is discussed, specifically what kinds of orbits are possible in galaxies described by a spherically symmetric, or an axially symmetric potential. Orbits in simply non-axisymmetric potentials will also be discussed.\nWe continue with a discussion of distribution functions and the equilibria of collisionless systems, and derive the collisionless Boltzmann equation. We then discuss the Jeans and virial equations and with the help of them detect black holes and dark matter haloes in galaxies using observations of the kinematics of their stars. This is followed by a discussion of the stability of collisionless systems. Next we discuss disk dynamics and spiral structure, followed by a discussion on kinetic theory and the thermodynamics of self-gravitating systems. We end the course with a discussion on dynamical friction and its applications and describe the related concepts of galaxy interactions and mergers." . . "Presential"@en . "FALSE" . . "Master's programme in Particle Physics and Astrophysical Sciences"@en . . "https://www.helsinki.fi/en/degree-programmes/particle-physics-and-astrophysical-sciences-masters-programme" . "120"^^ . "Presential"@en . "What are the laws of nature governing the universe from elementary particles to the development of the solar system, stars, and galaxies? In the Master’s Programme in Particle Physics and Astrophysical Sciences, you will focus on gaining a quantitative understanding of these phenomena.\n\nWith the expertise in basic research that you will gain in the programme, you might pursue a career in research. You will also acquire proficiency in the use of mathematical methods, IT tools and/or experimental equipment, as well as strong problem-solving and logical deduction skills. These will qualify you for a wide range of positions in the private sector.\n\nAfter completing the programme, you will:\n\n-Have wide-ranging knowledge of particle physical and/or astrophysical phenomena.\n-Have good analytical and computational skills and the ability to make sophisticated deductions.\n-Be able to apply theoretical, computational and/or experimental methods to the analysis and understanding of various phenomena.\n-Be able to apply your knowledge of particle physical and astrophysical phenomena as well as identify their interconnections.\n-Be able to formulate hypotheses and test them based your knowledge"@en . . . . "2"@en . "FALSE" . . . "Master"@en . "Thesis" . "no tuition, other costs may apply" . "Euro"@en . "15000.00" . "None" . "A Master’s degree in elementary particle physics or astrophysical sciences provides you with excellent qualifications for postgraduate education in research or for a career in diverse positions both in Finland and abroad. As a Master’s graduate you could begin a career in research and development in industry as well as in universities and other research institutes that enable you to conduct independent research on a topic that interests you."@en . "2"^^ . "TRUE" . "Upstream"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .