. "Astrophysics"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Data science in astrophysics"@en . . "8" . "no data" . . "Presential"@en . "TRUE" . . "Observational astrophysics: proposal preparation"@en . . "3" . "To work out small research projects in a team starting from a descriptive outline.\nTo synthesise the results of the research project in a scientific talk to the peers\nTo write a scientific report on the results of the conducted research\"" . . "Presential"@en . "TRUE" . . "Research projects in theoretical astrophysics"@en . . "3" . "to carry out small theoretical research projects in astrophysics and plasma astrophysics,\nto synthesizse the results of a project and to communicate the results in a scientific presentation\nto write a sceintific report about the background and the results of the research carried out" . . "Presential"@en . "TRUE" . . "Simulation and modeling in astrophysics (amuse)"@en . . "6" . "During this course you will learn how to perform research with existing computational tools and simulation codes. This will be done using the Astrophysics Multipurpose software Environment (AMUSE) software. You will learn how to set up a computer experiment, write the code to carry out the simulations, perform the calculations, collect and analyze the data, and critically assess the results.\n\nStudents, in groups of two or three, will work on their joined projects, and report on the results by written report and a presentation.\n\nThe final project is chosen in discussion with the teacher from a wide range of topics. From a computational point of view the topic should generally include at least two fundamental physical phenomena:\ngravitational dynamics, hydrodynamics, radiative transfer, or stellar astrophysics.\n\nThe work will be carried out using AMUSE to perform a number of simulations to study astrophysical phenomena. The course ends with a presentation and report on the final project.\n\nOutcome: Not Provided" . . "Presential"@en . "FALSE" . . "Numerical recipes in astrophysics"@en . . "6" . "In this course you will learn how and why some of the most powerful and broadly used algorithms in astrophysics work and gain a deeper understanding of numerical methods.This will allow you to identify the right tool for the job for whatever computational problem you may encounter in astrophysics, and to program more effectively, whether you are fitting data, sampling a distribution, integrating orbits or optimizing your computational model.\r\n\r\nDuring the lectures we will discuss numerics and consider and derive specific algorithms that are useful in astrophysics. During the problem classes students will work together on applying this knowledge to a computational problem through coding.\n\nOutcome:\nIn specific, after this course, you will be able to:\r\n\r\nEvaluate the outcomes of computational codes\r\nConstruct an efficient computer program\r\nSolve a wide array of astrophysical problems" . . "Presential"@en . "TRUE" . . "Simulation and modeling in astrophysics (amuse)"@en . . "6" . "During this course you will learn how to perform research with existing computational tools and simulation codes. This will be done using the Astrophysics Multipurpose software Environment (AMUSE) software. You will learn how to set up a computer experiment, write the code to carry out the simulations, perform the calculations, collect and analyze the data, and critically assess the results.\n\nStudents, in groups of two or three, will work on their joined projects, and report on the results by written report and a presentation.\n\nThe final project is chosen in discussion with the teacher from a wide range of topics. From a computational point of view the topic should generally include at least two fundamental physical phenomena:\ngravitational dynamics, hydrodynamics, radiative transfer, or stellar astrophysics.\n\nThe work will be carried out using AMUSE to perform a number of simulations to study astrophysical phenomena. The course ends with a presentation and report on the final project.\n\nOutcome: Not Provided" . . "Presential"@en . "FALSE" . . "Numerical recipes in astrophysics"@en . . "6" . "In this course you will learn how and why some of the most powerful and broadly used algorithms in astrophysics work and gain a deeper understanding of numerical methods.This will allow you to identify the right tool for the job for whatever computational problem you may encounter in astrophysics, and to program more effectively, whether you are fitting data, sampling a distribution, integrating orbits or optimizing your computational model.\r\n\r\nDuring the lectures we will discuss numerics and consider and derive specific algorithms that are useful in astrophysics. During the problem classes students will work together on applying this knowledge to a computational problem through coding.\r\n\r\nThe topics covered in the course include:\r\n\r\nNumerical error and precision\r\n\r\nSolving linear equations\r\n\r\nSolving differential equations\r\n\r\nInter- and extrapolation\r\n\r\nNumerical integration and differentiation\r\n\r\nRandom numbers and distribution sampling\r\n\r\nRoot finding, minimization and maximization\r\n\r\nFast Fourier transforms and applications\r\n\r\nModelling data\r\n\r\nOutcome:\nUpon completion of this course you will be able to judge which numerical algorithm or tool is right for any computational problem typically encountered in\r\nastrophysics.\r\n\r\nIn specific, after this course, you will be able to:\r\n\r\nEvaluate the outcomes of computational codes\r\n\r\nConstruct an efficient computer program\r\n\r\nSolve a wide array of astrophysical problems" . . "Presential"@en . "TRUE" . . "Theoretical astrophysics (1)"@en . . "7" . "Introduction (blackbody radiation, Stefan-Boltzmann law, specific intensity, flux, K-integral), Absorption and emission coefficient, Source function, Transfer equation (plane-parallel approximation, integral of flux, mean intensity and K-integral), Radiative equilibrium and Milne equations, Grey atmosphere (Eddington and Chandrasekhar solutions), Continuum absorption coefficient (absorption coefficients of hydrogen and helium, total absorption coefficient), Model atmosphere (hydrostatic equilibrium, temperature distribution, limb darkening, dependence on pressure and chemical composition), Line absorption coefficient (natural broadening, thermal broadening, pressure broadening, convolution, Fourier transformation, Voigt profile), Behavior of spectral lines (source function, profile), Chemical analysis and the line transfer equation, Stellar rotation, Turbulence in stellar atmospheres.\n\nOutcome:\nUnderstanding the basics of radiation transfer in stellar atmospheres." . . "Presential"@en . "TRUE" . . "Seminar on astronomy and astrophysics (1)"@en . . "2" . "Student's own scientific work, preparation of background materials and presentation of partial results of the diploma thesis. Active participation in the discussion. Presentation of current results of research programs by the staff of the Division of Astronomy and Astrophysics and invited speakers.\n\nOutcome:\nStudents will gain experiences with the preparation and oral presentation of their scientific work and with active participation in the discussion. Students will deepen their knowledge of the research fields covered at the seminar presentations." . . "Presential"@en . "TRUE" . . "Theoretical astrophysics (2)"@en . . "7" . "Introduction (definition of a star, HR diagram), Sources of stellar energy, Time scales, Conservation laws, The equations of stellar evolution, Properties of matter and energy transport (equation of state, electron degeneracy pressure, radiation pressure, adiabatic index, radiative transfer), Nuclear reactions (pp chain, CNO cycle, burning of He and heavy elements, s-process, r-process), Nuclear reaction rates and Gamow peak, Equilibrium stellar configurations (equations of stellar structure, polytrope, Chandrasekhar limit, Eddington luminosity), The stability of stars (thermal instability in degenerate gas, thin shell instability, dynamic instability, convection), Stellar evolution in rho-T diagram, An evolution of the stellar core and a structure of the star, The pre-main-sequence phase in HR diagram (protocloud, Jeans instability, fragmentation, Hayashi track), Stellar evolution on the main sequence (lower and upper part of the main sequence, Schönberg–Chandrasekhar limit), Evolution away from main-sequence in HR diagram (Hertzsprung gap, red giants, helium flash, helium core burning, AGB stars), Final stages of stellar evolution (white dwarfs, supernovae, neutron stars, black holes).\n\nOutcome:\nUnderstanding the basics of the theory of stellar structure and evolution." . . "Presential"@en . "TRUE" . . "Seminar on astronomy and astrophysics (2)"@en . . "2" . "The student will gain basic knowledge regarding the acquisition, processing and analysis of observation material.\n\nOutcome:\nStudents will gain experiences with the preparation and oral presentation of their scientific work and with active participation in the discussion. Students will deepen their knowledge of the research fields covered at the seminar presentations." . . "Presential"@en . "TRUE" . . "Solar physics"@en . . "4" . "Basic definitions and assumptions, basic physical facts about the Sun. Internal structure of the Sun, energy production, energy transfer by radiation and convection. The solar neutrinos problem. Helioseismology. Solar atmosphere. Photospheric radiation, radiative transfer in the photosphere, Fraunhofer spectral lines, photospheric structures. Chromosphere. Transition region and corona, optically thin radiation, solar flares, coronal mass ejections. Solar activity and its cycle, solar wind, solar-terrestrial connection, space weather. Magnetic fields in the solar atmosphere, measurements of the magnetic field strength, Stokes parameters. Solar dynamics, differential rotation and its description.\n\nOutcome:\nGain knowledge about the physics of the Sun and the physical processes of energy formation and transfer." . . "Presential"@en . "TRUE" . . "Seminar on astronomy and astrophysics (3)"@en . . "2" . "Student's own scientific work, preparation of background materials and presentation of partial results of the diploma thesis. Active participation in the discussion. Presentation of current results of research programs by the staff of the Division of Astronomy and Astrophysics and invited speakers.\n\nOutcome:\nStudents will gain experiences with the preparation and oral presentation of their scientific work and with active participation in the discussion. Students will deepen their knowledge of the research fields covered at the seminar presentations." . . "Presential"@en . "TRUE" . . "Seminar on astronomy and astrophysics (4)"@en . . "3" . "Student's own scientific work, preparation of background materials and presentation of partial results of the diploma thesis. Active participation in the discussion. Presentation of current results of research programs by the staff of the Division of Astronomy and Astrophysics and invited speakers\n\nOutcome:\nStudents will gain experiences with the preparation and oral presentation of their scientific work and with active participation in the discussion. Students will deepen their knowledge of the research fields covered at the seminar presentations." . . "Presential"@en . "TRUE" . . "Selected problems in astrophysics"@en . . "3" . "Basic terms, definitions, and processes. Planet detection methods. Cosmic missions. Exoplanet properties and observations. Special and famous exoplanets. Interior (convection, degeneracy, equations of the structure). Formation and evolution, radii. Atmospheres (irradiation, stratospheres, heat redistribution, chemistry and composition, dust...). Brown dwarfs (definitions, observations, properties, spectral classification MLTY, formation, disks, interior, evolution, atmospheres).\n\nOutcome:\nStudent will obtain basic knowledge required for further study and work in the field. Particular attention is given to understanding of the terms, methods and processes that take place in exoplanets and brown dwarfs. Course offers overview of the field with the latest highlights and discoveries." . . "Presential"@en . "FALSE" . . "Population of meteoroids"@en . . "3" . "All-sky astrometric reduction. Radians, velocities, calculation of meteoroid orbits, databases. Selection effects, sources of errors. Origin, structure and development of meteoroid streams, general characteristics, effects on meteoroids. Orbital similarity criteria and methods of distinguishing showers from sporadic background. Shower activity and mass inflow to Earth. Main meteor showers, minor showers, associations. Meteor storms. Activity modeling and predictions. Parent bodies of meteoroid strams, meteor complexes. Meteor showers of aasteroidal orgin. Sporadic population and its sources. Zodiacal cloud. Spatial structure and physical characteristics of individual components of the population. Geological periods, impact craters.\n\nOutcome:\nThe student will gain knowledge about research methods, structure and origin of the meteoroid population." . . "Presential"@en . "FALSE" . . "Astrophysics - state exams"@en . . "2" . "Blackbody radiation, Stefan-Boltzmann law, specific intensity, flux, K-integral, Absorption and emission coefficient, Source function, Transfer equation, Radiative equilibrium and Milne equations, Grey atmosphere, Continuum absorption coefficient, Model atmosphere, Line absorption, Behavior of spectral lines, Chemical analysis and the line transfer equation, Stellar rotation, Turbulence in stellar atmospheres. Sources of stellar energy, Time scales, Conservation laws, The equations of stellar evolution, Properties of matter and energy transport, Nuclear reactions, Nuclear reaction rates and Gamow peak, Equilibrium stellar configurations, The stability of stars (thermal instability in degenerate gas, thin shell instability, dynamic instability, convection), Stellar evolution in rho-T diagram, An evolution of the stellar core and a structure of the star, The pre-main-sequence phase in HR diagram, Stellar evolution on the main sequence, Evolution away from main-sequence in HR diagram, Final stages of stellar evolution.\n\nOutcome:\nThe students will proof the understanding of radiative transfer and the structure and evolution of stars." . . "Presential"@en . "TRUE" . . "Solar physics - state exams"@en . . "2" . "Basic definitions and assumptions, basic physical facts about the Sun. Internal structure of the Sun, energy production, energy transfer by radiation and convection. The solar neutrinos problem. Helioseismology. Solar atmosphere. Photospheric radiation, radiative transfer in the photosphere, Fraunhofer spectral lines, photospheric structures. Chromosphere. Transition region and corona, optically thin radiation, solar flares, coronal mass ejections. Solar activity and its\n\ncycle, solar wind, solar-terrestrial connection, space weather. Magnetic fields in the solar atmosphere, measurements of the magnetic field strength, Stokes parameters. Solar dynamics,\n\ndifferential rotation and its description.\n\nOutcome:\nStudents will demonstrate knowledge and ability to physically describe the interior and atmosphere of the Sun." . . "Presential"@en . "TRUE" . . "Computational methods for astrophysical applications"@en . . "6" . "The course starts with an introduction to common spatial and temporal discretization techniques to numerically solve sets of partial differential equations. Further on, the course treats various state-of-the-art numerical methods used in astrophysical computations. This encompasses basic shock-capturing schemes as employed in modern Computational Fluid Dynamics, common approaches for handling Radiative Transfer, and concrete gas dynamical applications with astrophysical counterparts. The main aim is to give insight in the advantages and disadvantages of the employed numerical techniques. The course will illustrate their typical use with examples which concentrate on stellar out-flows where the role and numerical treatment of radiative losses will be illustrated, but also touch on studies from solar physics, stellar atmospheres, astrophysical accretion disks and jets, pulsar winds, planetary nebulae, interacting stellar winds, supernovae . . . . The students will experiment with existing and/or self-written software, and gain hands-on insight in algorithms, their convergence rates, time step limitations, stability, .... The students will in the end be able to apply some of the schemes to selected test problems." . . "Presential"@en . "TRUE" . . "Computational methods for astrophysical applications"@en . . "6" . "no data" . . "Presential"@en . "FALSE" . . "Astrophysics"@en . . "5" . "Learning outcomes of the course unit:\nThe student will be able to mathematically rigorously describe various types of trajectories of planets and space probes in the solar system on the basis of physical laws. They will be able to analyze all significant effects affecting the stability of spacecraft orbits. The student will be able to determine and simulate the positions of bodies derived from their ephemeris. The student will gain the most important knowledge about the evolution of planetary systems and their central stars. The student will gain a sufficient general basis about the structure of galaxies and the organization of large-scale structures in space.Course Contents:\n• Newton's law of gravitation and Kepler's laws as starting points for the dynamics of gravitationally bound.\n• Classification of body trajectories in the spherically symmetric gravitational field of a central mass body.\n• The solar system as a gravitationally bound system of the Sun and its planets.\n• Basic types of spacecraft trajectories in the Solar System and the importance of gravity-assisted maneuvers.\n• Lagrange points in a system of two gravitationally coupled bodies. Significance of Lagrange points of the Sun-Earth system for observations and space research.\n• Electromagnetic interactions and their main effects in the space (light pressure, magnetic fields, cosmic plasma, etc.).\n• Ephemeris of objects (natural and artificial) and their meaning.\n• Calculation and simulation of the motion of artificial satellites in a real (not perfectly spherically symmetrical) gravitational field and under the influence of the most important perturbation influences (light pressure, remnants of the atmosphere).\n• Energy sources of stellar energy and strong interactions (pp and CNO cycle of thermonuclear fusion of stars of the main sequence)\n• The planets of the solar system, their main characteristics as the reflection of their distance from the Sun and the consequence of the planetary systems formation.\n• Physics of interplanetary and interstellar space and cosmic radiation.\n• Current knowledge about the structure and properties of galaxies and galaxy clusters. Rotational speeds of stars in spiral galaxies and other indirect signals of dark matter (motion of star clusters, gravitational lenses and large-scale fiber structures)." . . "Presential"@en . "FALSE" . . "Open problems in modern astrophysics"@en . . "5" . "LEARNING OUTCOMES\nThe student will familiarize him/herself with seven exciting hot topics in contemporary astrophysics.\nThe student will learn to read review papers and specialised research articles.\nThe student will learn how to interpret and understand the main results from a research article.\nThe student will learn how good research papers are written and how to best present scientific arguments.\nThe student will learn to discuss research articles, and how to present scientific points in a discussion.\nCONTENT\nDuring the course we will cover 7 different topics in modern astrophysics, with each topic discussed for two weeks. The new topic will first presented by the Lecturer based on a recent review paper typically published in the Annual Review of Astronomy and Astrophysics. During the second week the topic will be discussed in more depth by highlighting recent research articles in the relevant area. Finally, the topic will be rounded off by a problem set for which the students will have to read two research articles and answer questions based on the papers. The final exam will be a written exam in which the students will be asked questions about the various topics covered during the course at a general level and more in depth questions on a few chosen subjects.\n\nThe topics to be discussed during the course have been chosen to cover a broad range of astrophysics, including exoplanets, stars, galaxies and cosmology. In general the topics have been chosen to cover a broad range of astrophysics, including exoplanets, stars, galaxies and cosmology. The aim is to learn about interesting research topics that are likely to remain at the core of modern astrophysics in the coming decades. The exact content of the course will vary from year to year depending on what topics are considered particularly interesting for that year. In the previous year the following topics have been discussed: 1. The detection and properties of Extrasolar planets, 2. The formation and evolution brown dwarfs, 3. Gamma-Ray Bursts: Observation and Theory, 4. Massive black holes and gravitational waves, 5. Dwarf galaxies and structure formation, 6. The First Galaxies, 7. Dark Energy and the Accelerating Universe." . . "Presential"@en . "TRUE" . . "Small bodies in the solar system"@en . . "5" . "LEARNING OUTCOMES\nThe student knows where and how to find astronomical literature. The student is able to read and understand scientific literature, and can summarise the contents of scientific articles. The student can discuss scientific articles with his/her colleagues. The student understands the major research topics and their interconnections in small-body research and can provide an in-depth summary of the current status of asteroid research.\n\nCONTENT\nThe course starts with an introduction to asteroids and the history of asteroid research and proceeds to assess how remote observations yield information about asteroids. This part discusses, first, asteroid surveys, as well as numbers, orbits, biases, and size distributions of asteroids, and, second, physical properties such as sizes, shapes, spins, compositions, and thermophysical parameters of asteroids.\n\nThereafter, the discussion turns to dynamical, thermal, and collisional evolutionary processes affecting individual asteroids and groups of asteroids.\n\nTowards the end of the course, we consider interrelations between asteroids and other types of bodies in the Solar System including a discussion of asteroid families, relation of asteroids to meteoroid streams, evolution of comets into asteroids, main-belt comets, as well as the origins of the various populations of asteroids." . . "Presential"@en . "FALSE" . . "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" . . "High energy astrophysics"@en . . "5" . "LEARNING OUTCOMES\nThe students obtain the knowledge of the emission processes and particle acceleration mechanisms important for high-energy astrophysics. During the practical part, the students will learn how to reduce the modern high-energy observations.\n\nCONTENT\nEmission processes. Particle acceleration. Accretion disk. Sources of high energy radiation. High energy instrumentation.\n\nReduction of the high energy data." . . "Presential"@en . "FALSE" . . "Solar physics"@en . . "5" . "LEARNING OUTCOMES\nYou will learn about the history of formation of the Sun and its future evolution.\nYou will understand the processes of energy production and transfer in the Sun; the structure of the solar atmosphere, corona and solar wind; the generation and evolution of solar magnetic fields; and the physics behind the solar cycle, solar seismology, and solar storms.\nYou will learn about current and past solar space missions as well as ground observatories and will apply your knowledge to study various aspects of the Sun using real data.\nCONTENT\nFormation of the Sun and the solar system, future evolution of the Sun.\nStandard solar model.\nSolar atmosphere.\nSolar oscillations and helioseismology.\nConvection.\nSolar rotation.\nSolar dynamo and solar cycle.\nChromosphere and solar corona.\nSolar wind.\nSolar storms and eruptions." . . "Presential"@en . "FALSE" . . "High energy astrophysics"@en . . "7,5" . "The course covers the following areas: compact objects, mass transfer in binary systems, accretion discs,\nactive galactic nuclei, gamma-radiation bursts, cosmic radiation and acceleration mechanisms for relativistic\nparticles. It is expected that the student after taking the course will be able to: describe the most important radiation\nmechanisms and their observable aspects, and the dynamics of different types of compact objects - show\nunderstanding for the basic physics of accretion discs - describe different acceleration processes - describe the\nmost common relativistic effects of compact objects." . . "Presential"@en . "TRUE" . . "Astrophysical gas dynamics"@en . . "7,5" . "The course discusses the gas dynamic processes that are important in astronomy. It covers the basic equations\nthat describe gas motions, both with and without magnetic fields, shocks, turbulence, instabilities, gravity and\ngas, as well as an introduction to the numerical methods available to solve the gas dynamic equations. It is expected that the student after taking the course will be able to: know the gas dynamic equations and to\nunderstand their properties - solve simple problems in gas dynamics like, e.g., stationary solutions and shock\nsolutions - know the basic ideas behind numerical solutions to the gas dynamic equations - know and\nunderstand the most important types of instabilities - know the astrophysical applications of gas dynamics\nlike, e.g., accretion discs, stellar winds and explosions" . . "Presential"@en . "TRUE" . . "Fundamentals of astrophysics"@en . . "6" . "LEARNING OUTCOMES OF THE COURSE UNIT\n\nThe graduate of the course is able to describe and explain:\n- theory of gravity in the physical image of the world. Development of views on space, time and gravity.\n- Einstein's law of gravitation.\n- formal scheme of KM Principle of superposition in KM and its consequences.\n- description of planetary motion, Moon motion. Outline of solar and lunar eclipse calculations.\n- origin, evolution and final stages of stars, galaxies, quasars.\n- photometry. Radiation detectors - human eye, photographic emulsion, photomultiplier. Photoelectric photometers.\n- spectroscopy. Principles of spectroscopy. Optical prism and diffraction grating.\n\nCOURSE CURRICULUM\n\n1. Theory of gravity in the physical image of the world. Development of views on space, time and gravity. Principle of equivalence, its various formulations and corresponding experiments.\n2. Einstein's law of gravitation. Basic observational data about the universe as a whole - mass distribution, Hubble's relation, relic radiation, 'big bang'.\n3. Wave function - properties and interpretation. Operators of physical quantities - mean values, eigenvalues ​​and eigenfunctions.\n4. Formal scheme of KM Principle of superposition in KM and its consequences. States of microsystems as elements of vector space.\n5. Astrometry. Phenomena affecting coordinates - refraction, parallax, aberration, self-movement, precession, nutation. Instruments for terrestrial astrometry, interferometers, astrometric satellites. Doppler effect.\n6. Exact time. Stellar time, equations of equinoxes. Right and mean solar time, time equation. Atomic time, UT1 times, UTC, pole motion, motions of solar system bodies. Description of planetary motion, Moon motion. Outline of solar and lunar eclipse calculations.\n7. Calculation of trajectory elements from observed positions, units and quantities in astronomy and astrophysics. Electromagnetic radiation, laws of radiation of an absolutely black body.\n8. Origin, evolution and final stages of stars, galaxies, quasars. Classical methods of star observation. Spectral classification, luminosity classes, multidimensional classification, classification of variable stars and their places in HRD. Pulsating variable stars.\n9. Our Galaxy. Structure, kinematics and dynamics, rotation. Oort constants. Galactic core. Galaxies and quasars. Hubble classification of galaxies. Active galaxies and quasars. Optical systems of telescopes: Newton, Cassegrain, Gregory, Schmidt, Maksutov.\n10. Photometry. Radiation detectors - human eye, photographic emulsion, photomultiplier. Photoelectric photometers. Principle of CCD detector. Photometric systems and their applications. Ultraviolet and infrared photometry.\n11. Spectroscopy. Principles of spectroscopy. Optical prism and diffraction grating. Dispersion curve. Spectrograph. Microphotometer. Comparative spectrum. Unconventional spectroscopy. Atlases of spectra, tables of spectral lines. Spectrum processing - speed guidance.\n12. Radio astronomy. Antennas. Receivers. Point and area objects, continuous and linear radiation. Interferometry, aperture synthesis, VLBI. Radar equation. Ultraviolet, X-ray and gamma astronomy. Instruments of solar physics. Helioscopic eyepiece, whole state, solar spectrograph, coronograph\n13. Properties and detection of polarized light. Stokes parameters. Polarimeter, Wollaston polarizer\nAIMS\n\nThe aim of the course is for graduates to have a deeper overview of the basics of Astronomy and Astrophysics. Graduates will gain advanced knowledge in the major parts of classical and modern astronomy, astrophysics. They will also gain an overview of general areas of physics - theoretical mechanics, quantum physics, thermodynamics, statistical physics and general theory of relativity.\nThey will be able to define the basis of astrophysical phenomena and gain a general overview of the physical laws of the universe.\nThey will gain an overview of modern observation techniques and methods, they are ready for the analysis of observation data and the creation of numerical models." . . "Presential"@en . "TRUE" . . "Observational astrophysics I"@en . . "7,5" . "This course deals with fundamental concepts in observational astronomy/astrophysics. It teaches the concepts needed to plan and execute observations for scientific purposes, as well as for interpreting the resulting data. It is expected that the student after taking the course will be able to: know and understand the physical\nprocesses which give rise to detection of astronomical signals - know and understand the basic theory for the\ndescription of detection and imaging av astronomical signals - know and describe different types of\nastronomical observation systems, including optical systems and detectors - describe sources of noise and the\nresulting noise in the stochastic detection process, as well as estimate the signal-to-noise ratio and related\nintegration times for a given observation - show ability to independent gathering of knowledge about the\nphysical processes that are discussed, and in an independent way transmit this knowledge to other students\nand the teacher." . . "Presential"@en . "TRUE" . . "Observational astrophysics II"@en . . "7,5" . "The course prepares for practical work with the theoretical knowledge acquired in the course Astronomisk\nobservationsteknik I, AN, 7,5hp (AS7003). The practical work is done with an advanced telescope during one\nweek. The course gives knowledge and ability to write a complete observing time proposal, within which a\ndetailed estimate and report for the requested time is included, as well as a plan for observing the selected\ntargets. The course gives knowledge about the large software packages that control the telescope, the selected\ninstrument. It is expected that the student after taking the course will be able to: know and apply the extensive\ninformation needed to write an acceptable and competitive observing time proposal - know and understand\ntelescope and instrument parameters that are specific for a given observation of celestial objects - know and\npresent the signal-to-noise requirements given for the astronomical/astrophysical context on the one hand, and\nhow this can be realized at the telescope on the other - know and apply the available astronomical analysis\nsoftware and reduce the gathered data - in an independent way present this knowledge to other students and\nthe teacher." . . "Presential"@en . "TRUE" . . "astrophysics laboratory"@en . . "3" . "no data" . . "Presential"@en . "TRUE" . . "high-energy astrophysics"@en . . "3" . "1) Radiative transfer - including definitions of: emission and absorption coefficients, specific intensity, optical depth, flux density etc. We will discuss also different solutions of the radiation transfer equation. 2) Thermal radiation and the physical laws that describe this process. 3) Radiation of moving charges – Larmor’s formula and characteristic of this emission. 4) Transformation of the radiation (frequency, energy, angles etc.) from the particle comovig frame to the observer’s frame. 5) Different types of the bremsstrahlung process (thermal, relativistic). 6) From the cyclotron to the synchrotron emission – an useful approximations. 7) Synchrotron emission of a single particle. 8) Synchrotron emission produced by different types of particle energy distributions. 9) Synchrotron self-absorption process. 8) Thompson scattering. 9) Compton scattering. 10) Inverse Compton scattering. 11) Synchrotron self-Compton emission scenario. 12) External inverse-Compton emission scenario. 13) Particle acceleration – first and second order Fermi processes. 14) Evolution of particle energy spectrum." . . "Presential"@en . "TRUE" . . "astrohydrodynamics"@en . . "4" . "Part I. Astrophysical applications of fluid dynamics. - Euler’s equations of fluid dynamics, - selfgravitating fluids - Poisson’s equation - sound waves, shock waves, supernova explosions, - fluid instabilities: convective, Raileigh-Taylor, Kelvin-Helmholtz, gravitational and thermal instabilities, - Bernouli’s equation, spherical accretion and winds, - viscous flows, Navier-Stokes equation, Reynolds number, - vorticity equation, Kelvin’s theorem of vorticity conservation, - turbulence and its astrophysical significance, - hydrodynamics of accretion disks, - hydrodynamical processes in star formation activity. Part II. Numerical methods for fluid dynamics. - elements of the theory of partial differential equations, method of characteristics, Riemann problem, Rankine-Hugoniot relations, linear hyperbolic systems - conservative form of hydrodynamics equations, shock waves, rarefaction waves and the solution of Riemann problem in fluid dynamics. - basic numerical methods for partial differential equations, von Neuman stability analysis of numerical schemes, - Riemann solvers and Godunov methods for fluid dynamics." . . "Presential"@en . "TRUE" . . "theoretical astrophysics laboratory 1"@en . . "3" . "The student carries out the following topics in the form of tasks consisting of numerical calculations and report development. The following general topics are: - Solving ordinary differential equation systems using self-developed programs and software available in the public domain. - Solving partial differential equation systems using self-developed programs and software available in the public domain." . . "Presential"@en . "FALSE" . . "theoretical astrophysics laboratory 2"@en . . "3" . "The student carries out numerical calculations and writes reports. The proposed itopics are listed below, although alternatives are not excluded: - write from scratch a code that computes a model of a star using the polytropic equation of state - discuss late stages of stellar evolution using a publicly available stellar evolution code - analyze circumstellar material using a publicly available photoionization code" . . "Presential"@en . "FALSE" . . "theoretical astrophysics laboratory 3"@en . . "3" . "The computational projects will be realized with the aid of the magnetohydrodynamical code PIERNIK. Students perform and analyze a series of numerical experiments including: supernova explosions, accretion disks, astrophysical jets and selected hydrodynamical instabilities (gravitational instability, thermal instability, Kelvin-Helmholtz instability) of astrophysical relevance." . . "Presential"@en . "FALSE" . . "Introduction to astrophysics (not for bsc in astronomy)"@en . . "5" . "The topics covered by the course: Astronomical observations: contemporary astronomical instruments, observations at different wavelengths of radiation, physical processes related with emissions of radiation and particles Sun and other stars: fundamentals of stellar spectroscopy, basic knowledge of stellar structure and evolution, stellar life-cycles, synthesis and distribution of chemical elements, details of the structure of the Sun The Solar system and extrasolar planetary systems: contemporary knowledge of the Solar system, methods of searching and investigating extrasolar planets, orbital architectures, planet formation theories and astrophysical processes in circumstellar discs and environment, Earth-like planets Galaxies and the Universe: structure of the Universe at large scales, from galaxies through clusters and superclusters up to microwave background radiation and big-bang, theories of the evolution of the Universe Our place in the Universe: Earth and celestial sphere, importance of astronomy for science and philosophy, life in the Universe" . . "Presential"@en . "FALSE" . . "Exploring the solar system"@en . . "no data" . "no data" . . "Presential"@en . "FALSE" . . "Stellar astrophysics & astronomical techniques"@en . . "no data" . "Learning Outcomes:\r\nOn completion of this module students should be able to:\r\n(1) describe the techniques and results of observations of stars\r\n(2) derive/calculate information about stars' physical properties from the measurement data\r\n(3) apply the laws of physics to understand the properties and evolution of stars, and apply models to determine parameters such as central pressure, central temperature, lifetime etc.\r\n(4) describe the processes of stellar nucleosynthesis\r\n(5) describe the compact objects that form at the end of stars' lives, including White Dwarf stars, Neutron stars and Pulsars.\r\n(6) discuss the detection methods and techniques used by astronomical telescopes for operation in different parts of the electromagnetic spectrum, and perform basic calculations of telescope performance and sensitivity\r\n\r\nIndicative Module Content:\r\nRough outline of the course\r\n\r\n- Introduction: stellar properties (distances, magnitude, luminosities, etc); The HR diagram; ...\r\n\r\n- Stellar structure\r\n\r\n- Stellar evolution\r\n\r\n- Astronomical techniques: Earth atmosphere; Fundamental concepts; Telescopes" . . "Presential"@en . "FALSE" . . "Theoretical astrophysics"@en . . "no data" . "On successful completion of this module a student will (1) understand the principles of astrophysical radiative processes and gas dynamics, (2) understand how fundamental areas of physics combine in different astrophysical settings, (3) solve problems in radiative processes and gas dydnamics and (4) explain select astronomical observations using the tools of theoretical astrophysics." . . "Presential"@en . "FALSE" . . "Introduction to theoretical astrophysics"@en . . "5" . "no data" . . "Presential"@en . "FALSE" . . "Introduction to astrophysics"@en . . "5" . "no data" . . "Presential"@en . "TRUE" . . "Computational astrophysics"@en . . "5" . "no data" . . "Presential"@en . "TRUE" . . "Astrophysics I"@en . . "5" . "Introduction, basic definitions, stellar parameters: Astronomy as an observational science,\nastrophysics. Celestial sphere, coordinate systems used in astronomy. Stellar parallax,\ncosmic distance scale, distance ladder. Blackbody radiation. Stellar spectra, flux, effective\ntemperature. Spectral classification. Magnitude scale, bolometric magnitude, luminosity,\ncolour index. Stellar parameters. Determination of stellar masses and radii. Hertzsprung-\nRussell diagram. Tools of astrophysics: Electromagnetic spectrum, observing windows.\nGround-based and space observatories. Telescopes. Detectors. Infrared, ultraviolet, X-ray\nand gamma astronomy. Observing techniques: imaging. Observing techniques: photometry.\nObserving techniques: spectroscopy. Observing techniques: optical and radio interferometry.\nObserving techniques: astrometry. Observing techniques: polarimetry. Stellar atmospheres:\nDescription of radiation field. Interaction of light and matter, stellar opacity. Radiative and\nconvective transfer. Transfer equation and its formal solution. Equations of hydrostatic and\nradiation equilibrium. Gray atmosphere, diffusion approximation, LTE approximation. Models\nof stellar atmospheres. Spectral lines and their profiles, formation of spectral lines.\nAtmospheric abundances of stars. Ages of stars. Stellar structure and evolution: Interstellar\nmatter (IM), dust and gas, absorption by IM. Formation of stars, virial theorem, the Jeans\nmass. Pre-main sequence evolution. Stellar interiors, hydrostatic equilibrium. Basic\nequations. Sources of stellar energy, opacity, equation of state, transport of energy. Models\nof stellar interiors. Degeneracy of matter. Main-sequence evolution. Post-main-sequence\nevolution. Testing the theory of stellar evolution (stellar clusters, stellar pulsations). Stellar\nvariability and its origin. The Sun: Solar interior. Solar atmosphere. Activity of the Sun, solar\ncycle. Solar pulsations. Solar neutrino problem." . . "Presential"@en . "TRUE" . . "Modern trends in astrophysics I4 or selected topics in astrophysics I4"@en . . "1" . "Presentation and discussion of recent achievements and main research trends in the field of modern astrophysics, including the impact of astrophysics discoveries on our understanding of the world and the progress of science, as well as their civilizational significance." . . "Presential"@en . "TRUE" . . "Introduction to solar physics"@en . . "2" . "Solar interior, distribution of physical parameters and chemical composition of solar plasma,\nthe neutrino problem. Interaction of magnetic field with plasma, basics of\nmagnetohydrodynamics of the solar phenomena, solar dynamo. Activity of the Sun; short\nand long term solar variability. Solar atmosphere. Quiescent and active structures in the solar\nchromosphere and corona. Solar eruptions and ejections. Sun-Earth connections. Space\nWeather. Solar wind. Modern space and ground-based solar telescopes and observing\ntechniques. Multi-wavelength imaging and spectroscopic methods." . . "Presential"@en . "TRUE" . . "Laboratory of theoretical astrophysics / laboratory of magnetic activity of the sun and stars"@en . . "3" . "Introduction to MESA stellar evolution code. Description of the possibilities and limitations of \nthe program. Calibration of numerical parameters in order to obtain results that make \nphysical sense. Learning how to model different astrophysical objects: molecular clouds\ncontracting on the main sequence, main sequence stars, red giants, AGB stars, horizontal \nbranch stars, white dwarfs, black holes. Analysis of physical processes in different phases of \nstellar evolution (nuclear reactions, convection, diffusion of chemical elements, energy \ntransport, mass loss, mixing of matter, angular momentum transport). Modeling the \nevolution of binary systems with mass exchange between the components./ Calibration methods for spectroscopic observations of solar flares and prominences obtained \r\nin the optical range. Ultraviolet spectroscopy and photometry of active solar phenomena. \r\nTemporal evolution of stellar and solar flare emissions. Strategies and methods used in the \r\nmodelling of solar and stellar flares. One-dimensional models of the active atmosphere of the \r\nSun and stars. Distributions of non-thermal electrons in the flaring loop (Fokker-Planck). \r\nDiagnostics of star spots based on the photometric modulations. Analysis of solar and stellar \r\nactivity cycles. Detection of stellar flares in global surveys of the sky." . . "Presential"@en . "FALSE" . . "Astrophysics II"@en . . "5" . "Final stages of stellar evolution: Core-collapse supernovae. Neutrino astronomy. White\ndwarfs. Physics of degenerated matter. Chandrasekhar limit. Neutron stars, pulsars. Stellar\nblack holes. Gamma-ray bursts. Cosmic rays, Cerenkov telescopes. Close binary stars:\nEvolution of binary stars. Accretion disks. Tidal phenomena. Type Ia supernovae. Stellar\nmergers. Gravitational waves and their detection. Solar System, extrasolar planets: Solar\nSystem, planets. Elements of celestial mechanics (orbits, Kepler laws). Small bodies in the\nSolar System. Formation of planets. Extrasolar planets, detecting techniques. Evolution of\nplanetary systems. Galaxies: The Milky Way Galaxy (components, kinematics, the central\nsupermas-sive black hole). Types of galaxies and their parameters. Formation and evolution\nof galaxies. Active galactic nuclei and quasars. The large-scale structure of the Universe.\nGravitational lensing. Cosmology: Friedmann equations. Cosmological models, their\nparameters and testing. Expansion of the Universe and its acceleration. Early Universe.\nInflation. Primordial nucleosynthesis. Microwave background radiation. Dark matter and dark\nenergy. Theories of modified gravity." . . "Presential"@en . "TRUE" . . "Highlights of modern physics and astrophysics"@en . . "3" . "Presentation and discussion of selected topics of modern physics and astrophysics, with \nemphasis placed on major achievements, groundbreaking discoveries and leading trends of \ncurrent research, as well as the impact of astrophysical research on science and civilization.\nReview of literature and other sources on a given topic, preparing an abstract of oral \npresentation, delivering a talk, scientific discussion, writing an essay." . . "Presential"@en . "TRUE" . . "Practical astrophysics at observatory5"@en . . "2" . "Heliophysical part: Getting acquainted with the heliophysical instrumentation located at the \nAstronomical Observatory in Bialkow – Large Coronagraph (LC), Horizontal Telescope (HT), \nMulti-channel Subtractive Double-Pass spectrograph (MSDP spectrograph). Presentation of \nthe principle of operation of the MSDP imaging spectrograph. Spectroscopic heliophysical \nobservations in the hydrogen H-alpha spectral line, by the use both solar telescopes (LC, HT) \nand the MSDP imaging spectrograph. Theoretical introduction to the physics of solar active \nphenomena observed at the Bialkow Observatory (solar flares, prominences, filaments, \neruptions). MSDP data processing and analysis of active phenomena recorded during \nobservations at the Bialkow Observatory. Spectral analysis of the hydrogen H-alpha line \nduring various active phenomena observed on the Sun. Astrophysical part: Acquaint to the \nobservation site and observational instruments. Construction of the telescope located at the \nAstronomical Observatory in Bialkow: optics, mount, CCD detector, filter wheel, autoguider, \ntelescope control, and operation of the observational dome. An introduction to astrophysical \nobservations: observation conditions, small and large ground-based telescopes, space \ntelescopes, photometry, spectroscopy. General discussion of the observation technique used \nat the astrophysical observatory of the University of Wrocław: multicolor photometry, \ndifferential photometry, and photometric time series. Summary of the research subjects \nstudied at the astrophysical observatory of the University of Wrocław: multicolor photometry \nof star clusters (open and globular clusters), color-magnitude diagrams, photometric \nvariability of stars (pulsating stars, eclipsing stars, irregular variables). Discussion and \n(partial) execution of a typical course of astrophysical observations: calibration frames \n(images before and after calibration), observations of selected objects, ways of performing \nof photometric measurements, and a light curve." . . "Presential"@en . "TRUE" . . "Stellar pulsations"@en . . "5" . "Basic concepts and mathematical issues: oscillation mode, radial and non-radial pulsations,\nspherical harmonics, basic coordinate systems and transformations between them, the\nEulerian and Lagrangian description, perturbation of the surface element and its normal.\nTypes of pulsating variables: stellar pulsations across the Hertzsprung-Russell diagram,\ninstability domains, basic properties of different types. Oscillation properties: the Lamb and\nBrunt-Vaisala frequency, acoustic and gravitational modes, propagation diagrams, conditions\nfor trapping of modes, pulsation constant, period-luminosity relation. Mathematical\ndescription of pulsations: general equations of hydrodynamics, linear non-radial non-\nadiabatic pulsations, boundary conditions, adiabatic and quasi-adiabatic approximation,\nSturm-Liouville type problem, variational principle, asymptotic dispersion relations.\nExcitation mechanism: Eddington valve mechanism, self-excitation (opacity) mechanism,\nwork integral, stochastic excitation by turbulent convection. Detection of pulsating stars:\nFourier methods, statistical methods, wavelet analysis. Observed characteristics and\nidentification of pulsation modes: light variations of a pulsating star, changes of radial\nvelocity, modelling of line profile variations, methods of the mode identification from\nphotometry and spectroscopy. Basic effects of rotation: advection, rotational splitting of\nmodes, Coriolis force, Ledoux constant, effects of moderate rotation, centrifugal force. Helio-\nand Asteroseismology: seismic model of a star, the most important achievements of\nhelioseismology, examples of asteroseismic modelling." . . "Presential"@en . "TRUE" . . "Relativistic astrophysics"@en . . "6" . "Introduction: planets, stars, galaxies – scales and units. Reviewing statistical mechanics and\nintroducing the concept of an equation of state – equilibrium physics. Describing structure\nand evolution of stellar objects using the concept of hydrostatic equilibrium; Newtonian and\ngeneral relativistic approaches. Understanding the decoupling of radiation from matter to\ndescribe stellar atmospheres – opacity and mean-free path." . . "Presential"@en . "FALSE" . . "Modern trends in astrophysics Iv4 or selected topics in astrophysics Iv4"@en . . "1" . "Presentation and discussion of recent achievements and main research trends in the field of \nmodern astrophysics, including the impact of astrophysics discoveries on our understanding \nof the world and the progress of science, as well as their civilizational significance." . . "Presential"@en . "TRUE" . . "High-energy astrophysics"@en . . "5" . "Physical quantities and units used in high-energy Astrophysics. Observation techniques\n(detectors, Voltaire optics, aperture modulated telescopes). X-ray and gamma astronomy\n(development of techniques for recording and analysing satellite data). Electromagnetic\nprocesses in matter (Coulomb scattering, ionisation losses, braking radiation, thermal\nbremsstrahlung). Interaction of radiation with matter and magnetic field (Cherenkov\nradiation, Compton scattering, inverse Compton effect, synchrotron radiation, synchrotron\nabsorption, synchrotron-self-compton radiation, formation of electron-positron pairs,\npositron and electron annihilation). Accretion disks (accretion efficiency for white dwarfs and\nneutron stars, accretion efficiency for black holes for Schwarzschild and Kerr metrics,\naccretion types, Eddington luminosity limit, black holes in X-ray binaries and AGN, thin\naccretion disks, thick accretion disks, powering the accretion disk, influence of the magnetic\nfield on the accretion disk). Cosmic rays (composition of cosmic rays, energy spectrum,\nmodulation of cosmic rays, chemical content of elements in cosmic rays, the highest energies\nof cosmic rays, Great Atmospheric Air Showers (electromagnetic and muon cascades),\nrecording methods, observation projects, distribution of cosmic rays, energy density,\nGreisen-Zatsepin-Kuzmin cutoff). Neutrino astronomy (description of neutrino properties,\nastrophysical sources of neutrinos, detection of neutrinos, observations of solar neutrinos\nand the problem of their quantity, neutrino oscillations, other neutrino sources, cosmic rays\nand the Earth's atmosphere, supernova explosions (neutrino formation mechanism and\nobservations), AGN – mechanisms of neutrino formation). Gamma-ray bursts (observation\nproperties, determination of distances, burst formation sites, proposed models, observation\nof kilonova phenomena - detection of gravitational waves, distances, masses, detection of\ngamma rays)." . . "Presential"@en . "FALSE" . . "Theoretical astrophysics 1-4"@en . . "10" . "Semester 1: Physical foundaions\nThermodynamics: ideal gas, parial ionisaion, Saha equaion. Degeneraion of mater. Nuclear reacions. Basics of luid mechanics and magnetohydrodynamics. Linear perturbaions, waves in homogeneous media, perturbaions in straiied media. Turbulence and convecion. Radiaive transfer equaion\n\nSemester 2: Stellar structure and evoluion\nApplicaion of luid mechanics to stars. Thermodynamics of stellar plasma. Radiaive and convecive transfer of energy. Simpliied models, polytropic spheres. Numerical methods in the modelling of steallr structure and evoluion. Stability of stars: theory of linear pulsaion. Basics of numerical modelling of nonlinear pulsaions. Introducion to asteroseismology. Stellar evoluion: energy producion and nucleosynthesis. Phases of stellar evoluion.\n\nSemester 3: Radiaive transfer\nSaha equaion, Fowler-Milne theory of stellar spectra. Radiaive equilibrium in stellar atmospheres. Transfer equaion. Limb darkening. Theory of Fraunhofer lines. Mechanisms of absorpion, damping, Doppler broadining. Theory of the growth curve, determinaion of stellar composiion. Nontehrmal radiaion processes: synchrotron radiaion, nonthermal bremsstrahlung, comptonisaion.\n\nSemester 4: Difuse matter\nRadiative transfer and raditaive processes in difuse media. Interstellar molecules. The luid dynamics of difuse mater, shock waves. Interstellar dust and gas. Interstellar magneic ields. Interstellar medium in the Milky Way Galaxy. Star formaion. Planetary nebulae and supernove remnants." . . "Presential"@en . "TRUE" . . "Astrophysics 1-2"@en . . "4" . "Semester 1: Elements of potenial theory,: shell theorems, virial theorem, Poisson equaion. Basics of cosmology. Elements of radiaive transfer. Thermal radiaion. Random walk, difusive approximaion, transport coeicients, Rosseland opacity. Equaions of stellar structure. Overview of stellar evoluion.\n\nSemester 2: Eddington's criical luminosity. Stellar winds and driving mechanisms. Parker's solar wind model. Spherical (Bondi) accreion. Scatering in 1/r potenial. Applicaion to plasmas: transport coeicients. Applicaion to stellar systems: stellar encounters, collisional relaxaion. Basics of stellar dynamics. Elements of gravitaional lensing. Free-free transiions, bremsstrahlung. Thermal bremsstrahlung. Elements of the theory of accreion, thin accreion disks, Shakura-Sunyaev model." . . "Presential"@en . "FALSE" . . "High-energy astrophysics"@en . . "6" . "Course Content\r\n1. Introduction to high-energy Universe: astrophysical objects & observational methods\r\n\r\n2. Gas dynamics, accretion flows, Bondi accretion, Roche lobe overflow & accretion discs\r\n\r\n3. Radiation mechanisms: Bremsstrahlung, synchrotron & inverse Compton radiation\r\n\r\n4. Supernova remnants, astrophysical shocks & particle acceleration\r\n\r\nALGEMENE COMPETENTIES\r\n1. Knowlegde of the astrophysical objects and observational methods of the high-energy Universe.\r\n\r\n2. Understanding of gas dynamics, accretion flows and shocks.\r\n\r\n3. Understanding of Bremstrahlung, synchrotron emission and Inverse Compton scattering in an astrophysical context.\r\n\r\n4. Understanding of particle acceleration in astrophysical shocks." . . "Presential"@en . "TRUE" . . "Radiative transfer simulations in astrophysics"@en . . "6" . "• Interstellar dust: formation and destruction, shapes, size distribution, optical and calorimetric\r\n• properties.\r\n• The radiative transfer equation: derivation, source and sink terms, line and continuum\r\n• transport, scattering by dust, dust absorption and re-emission in local equilibrium conditions.\r\n• The photon package life cycle: Monte Carlo basics, primary emission, interactions with the\r\n• dust, escape and detection, panchromatic simulations and dust emission.\r\n• Spatial grids: grid traversal, regular Cartesian grids, hierarchical grids, Voronoi grids.\r\n• Sampling from spatial distributions: random number generators, inversion method, rejection\r\n• method, decorating geometries with spiral arms or clumps, importing hydrodynamics\r\n• simulation results.\r\n• Optimization techniques: forced scattering, continuous absorption, peel-off, composite\r\nCredits 6.0 Study time 180 h\r\nTeaching languages\r\nKeywords\r\nPosition of the course\r\nContents\r\nCourse size (nominal values; actual values may depend on programme)\r\n(Approved) 1\r\nAccess to this course unit via a credit contract is determined after successful competences assessment\r\nThis course unit cannot be taken via an exam contract\r\nend-of-term and continuous assessment\r\nexamination during the second examination period is not possible\r\nAssignment\r\nGroup work, lecture, independent work\r\n• biasing.\r\n• Parallelization: shared and distributed memory, redistribution of parallel data between\r\n• simulation phases, performance scaling.\r\n• Inverse radiative transfer: fitting analytical models to observations, searching large parameter\r\n• spaces.\r\n• Extensions to the basic radiative transfer equation: dust heating in nonequilibrium conditions,\r\n• polarization, kinematics, radiation hydrodynamics.\r\n• Other radiative transfer simulation techniques: ray-tracing, moment method, dealing with high\r\n• optical depth, benchmark efforts.\r\nSeveral of these subjects are illustrated with astrophysical science cases, and the\r\naccompanying practical project links directly into many of the theoretical subjects.\nFinal competences:\n1 Derive the radiative transfer equation and understand its components.\r\n2 Describe the Monte Carlo photon package life cycle and related techniques for spatial discretization, sampling from three-dimensiomal distributions, computational optimization, and parallelization.\r\n3 Explain the pros and cons of the various techniques used in radiative transfer simulations.\r\n4 Describe some science cases to which to radiative transfer simulations are applied and\r\n1 explain why they are relevant.\r\n5 Apply a state-of-the-art radiative transfer code to basic science cases.\r\n6 Adjust a scientific code written in C++ to specific research demands.\r\n7 Interpret radiative transfer simulation results in a numerical and astrophysical context.\r\n8 Orally convey the findings of a radiative transfer simulation project to experts." . . "Presential"@en . "FALSE" . . "Computational astrophysics and statistics"@en . . "8" . "The aim of the course is to provide knowledge and understanding of the fundamental numerical techniques currently employed in astrophysical simulations. The student will learn to solve ordinary and partial derivatives differential equations describing interesting astronomical problems. At the end of the course the student will be able to design and run simple numerical simulations of gasdynamical and N-body astronomical problems. A main goal of the class is to accustom the students to research fields which heavily use simulations and to understand merits and caveats of such studies." . . "no data"@en . "TRUE" . . "Astrophysics of galaxies"@en . . "6" . "The course addresses in depth some fundamental topics of the astrophysics of galaxies, training the students to analyze and critically discuss papers relevant for the current research in the field. Starting from a dynamical description of the structure of galaxies, the course then examines the comparison between model and observed quantities, in particular acquired with recent observational campaigns; the evidence for dark matter, extended and in the form of central massive black holes; the properties of the hot interstellar medium; the physical origin of the main galaxy scaling laws." . . "no data"@en . "FALSE" . . "High energy astrophysics"@en . . "6" . "This course focuses on the description of mechanisms and physical processes responsible for the emission observed from populations of Galactic and extra-galactic sources in the high-energy portion of the electromagnetic spectrum (mostly X-ray and Gamma-ray). All the phenomena will be illustrated using results from state-of-the-art X-ray and Gamma ray observatories. Students will be able to critically comprehend and discuss the high-energy emission properties of different classes of cosmic sources (e.g. compact X-ray sources such as X-ray binaries and Active Galactic Nuclei, clusters of galaxies, exploding stars such as Supernovae and Gamma Ray Burst, the Galactic Center). Through a multi-wavelength (and multi-messenger) approach, students will be able relate the X-ray properties of the observed sources with their emission at other wavelengths (and other messengers). The student is expected also to attain a basic knowledge of the techniques related to the detection of X-ray and Gamma-ray photons and on the properties of past, present, and future X-ray telescopes." . . "no data"@en . "FALSE" . . "High performance computing for astrophysics and cosmology"@en . . "6" . "The students will acquire the basic concepts of algorithm parallelisation and the practical skills to implement a parallel code using different parallelisation strategies. The methods to test the computational efficiency of a parallel algorithm and to assess its performance in terms of scaling, work load, and memory consumption will be presented. Furthermore, the students will learn the basic techniques for handling, monitoring, and exploiting the use of shared computational architectures ranging from small computer clusters to large supercomputing facilities. The laboratory part of the course will focus on some selected applications of these methods to standard astrophysical and cosmological problems" . . "no data"@en . "FALSE" . . "Magnetic fields in astrophysics"@en . . "6" . "During the course, the student will learn the basics of magnetised plasma in astrophysics. The origin of magnetic fields in the primordial Universe as well as the magnetic field properties of astrophysical objects will be discussed. The student will also learn the main techniques to derive magnetic field properties in astrophysical objects from observations. During the laboratory, these techniques will be used by the student using real data." . . "no data"@en . "FALSE" . . "Practical statistics for physics and astrophysics"@en . . "6" . "Nontrivial data analysis problems are frequently encountered in modern astronomy, cosmology and physics. They require an understanding of statistical methods, practical skills with software tools and sometimes some ingenuity that comes with experience. The student will gain a practical knowledge of statistical methods and software as applied to many example problems. Basic probability theory will be covered before learning about Bayesian and frequentist inference problems, Monte Carlo techniques, Fisher matrices, parameter estimation, non-parametric tests, hypothesis testing, and supervised and unsupervised classification and regression problems. The student will become familiar with current software in Python for analysing data and fitting models while getting an understanding of the theory behind them." . . "no data"@en . "FALSE" . . "Multiwavelength astrophysics laboratory"@en . . "8" . "At the end of the course students will acquire knowledge about reduction, analysis and interpretation of data from ground-based and space-based facilities across a wide range of wavelengths, from radio (centimeter and millimeter) to optical/near-IR and X-rays/Gamma-rays. Modern techniques of astronomical data analysis will be acquired by the student, along with the capability of presenting and discussing professionaly the results of the analysis of measurements taken during the course." . . "no data"@en . "FALSE" . . "Astrophysics"@en . . "no data" . "no data" . . "no data"@en . "TRUE" . . "Modern astrophysics"@en . . "9" . "not available" . . "Presential"@en . "TRUE" . . "Big data, ml and astrophysical data-sets"@en . . "9" . "not available" . . "Presential"@en . "TRUE" . . "Numerical methods in astrophysics"@en . . "9" . "not available" . . "Presential"@en . "TRUE" . . "High energy astrophysics"@en . . "6" . "I - Introduction to high-energy astrophysics and instrumentation\r\nIa - Detection techniques for high-energy photons. X-ray and Gamma-ray detectors. Wolter-type telescopes and coded-aperture masks. Cherenkov radiation.\r\nIb - History of high-energy astrophysics and properties of the main X-ray and Gamma-ray observatories.\r\nIc - Main physical parameters describing the accretion of matter onto compact objects: radial and disk accretion, mass transfer, radiative efficiency, Eddington luminosity, outflows.\r\nId - Brief description of the main emission mechanisms in high-energy astrophysics. Blackbody, bremsstrahlung, synchrotron, Compton scattering and inverse Compton scattering. Collisional ionization and photoionization, line emission and absorption.\r\n\r\nII - Galactic high-energy sources\r\nIIa - Compact sources: X-ray emission from stars in the main-sequence and pre main-sequence. White dwarfs, cataclysmic variables, novae, pulsars, pulsar wind nebulae, and neutron stars. Physical properties of accreting neutron stars and stellar mass black holes. Classification of X-ray binaries.\r\nIIb - Diffuse sources: Supernova remnants. The Galactic center region and the high-energy emission related to SgrA*. Fermi Bubbles.\n\r\nIII - Extragalactic high-energy sources\r\nIIIa - Compact sources: Active galactic nuclei (AGN), quasars, blazars. Electromagnetic counterparts of astro-particle sources. Ultraluminous X-ray sources (ULXs).\r\nIIIb - Diffuse sources: Starburst galaxies. Cluster of galaxies." . . "Presential"@en . "FALSE" . . "Data analysis and modeling in geoscience and astrophysics"@en . . "5" . "The course deals with methods for data representation and quality assessment, parameterization of physical systems, description of empirical and analytical relationships between data and model parameters, stochastic description of uncertainties and noise, and stochastic and deterministic quantification of prior knowledge about a physical system.\r\n\r\nA number of analytical/numerical methods for solving linear and nonlinear inverse problems are presented. The propagation of noise in the data to uncertainty of the solutions is a major theme in the course." . . "Presential"@en . "FALSE" . . "Astrophysical data analysis"@en . . "5" . "To give the students a working knowledge of astronomical data acquisition, analysis, and scientific exploitation. The course will train students in using professional software and tools to analyze real astronomical data from a series of different wavelengths and telescopes." . . "Presential"@en . "FALSE" . . "Observational x-ray astrophysics"@en . . "5" . "To give an introduction to X-ray astrophysics, its methods, its objects, and the involved physical processes." . . "Presential"@en . "FALSE" . . "Astrophysics"@en . . "6" . "Objectives: Study of the solar system and beyond, putting to application the tools previously acquired in\nthe general physics modules: Solar System • Planetary motion • Sources of radiation in astrophysics • Astrophysics without photons • Stellar structure • Stellar formation and evolution" . . "Presential"@en . "TRUE" . . "Astrophysics"@en . . "no data" . "no data" . . "Presential"@en . "FALSE" . . "Astrophysics"@en . . "no data" . "no data" . . "Presential"@en . "FALSE" . . "High energy astrophysics"@en . . "6" . "Not found" . . "Presential"@en . "TRUE" . . "Ionized nebulae"@en . . "6" . "Specific Competition\nCE1 - Understand the basic conceptual schemes of Astrophysics\nCE4 - Understand the structure and evolution of galaxies\nGeneral Competencies\nCG2 - Understand the technologies associated with observation in Astrophysics and instrumentation design\nCG4 - Evaluate the orders of magnitude and develop a clear perception of physically different situations that show analogies allowing the use, to new problems, of synergies and known solutions\nBasic skills\nCB6 - Possess and understand knowledge that provides a basis or opportunity to be original in the development and/or application of ideas, often in a research context\nCB7 - That students know how to apply the knowledge acquired and their ability to solve problems in new or little-known environments within broader contexts\nCB8 - That students are able to integrate knowledge and face the complexity of formulating judgments based on information that, being incomplete or limited, includes reflections on the social and ethical responsibilities linked to the application of their knowledge and judgments\nCB10 - That students possess the learning skills that allow them to continue studying in a way that will be largely self-directed or autonomous\nExclusive to the Specialty in Observation and Instrumentation\nCX8 - Understand the structure and evolution of nebulae and other large objects\n6. Subject contents\nTheoretical and practical contents of the subject\n1. INTRODUCTION\n2. IONIZATION BALANCE: Nebula of pure H. H and He nebula. Presence of heavy elements. Ionization parameter.\n3. THERMAL EQUILIBRIUM: Energy gain by photoionization. Cooling processes. Collisional excitation lines. Resulting thermal balance.\n4. SPECTRUM OF A NEBULA: Optical recombination lines. Continuous spectrum in the optic. Continuous spectrum and lines in radio. Radiation transport and collisional excitation effects on the lines. Fluorescence.\n5. CALCULATION OF PHYSICAL CONDITIONS AND CHEMICAL ABUNDANCES: Correction for redness due to dust. Electronic temperature and density. Chemical abundances. Empirical calibrations for determining abundances. Analysis of ionizing stellar radiation and calculation of other magnitudes.\n6. TYPES OF PHOTOIONIZED NEBULAS: HII regions. Planetary Nebulae. Nova Shells. Supernova Remnants." . . "Presential"@en . "FALSE" . . "Computational astrophysics"@en . . "6" . "Specific Competition\nCE8 - Know how to program, at least, in a relevant language for scientific calculation in Astrophysics\nCE11 - Know how to use current astrophysical instrumentation (both in terrestrial and space observatories) especially that which uses the most innovative technology and know the fundamentals of the technology used\nGeneral Competencies\nCG1 - Know the advanced mathematical and numerical techniques that allow the application of Physics and Astrophysics to the solution of complex problems using simple models\nBasic skills\nCB6 - Possess and understand knowledge that provides a basis or opportunity to be original in the development and/or application of ideas, often in a research context\nCB7 - That students know how to apply the knowledge acquired and their ability to solve problems in new or little-known environments within broader contexts\nCB8 - That students are able to integrate knowledge and face the complexity of formulating judgments based on information that, being incomplete or limited, includes reflections on the social and ethical responsibilities linked to the application of their knowledge and judgments\nCB10 - That students possess the learning skills that allow them to continue studying in a way that will be largely self-directed or autonomous\nExclusive to the Theory and Computing Specialty\nCX2 - Apply knowledge of computer science, physics, astrophysics and computing to build numerical simulations of astrophysical phenomena or scenarios\n6. Subject contents\nTheoretical and practical contents of the subject\n\n- Topics (headings):\n\n1. COMPUTER SIMULATION AND \"MACHINE LEARNING\" METHODS AS TOOLS IN ASTROPHYSICS.\n\n2. NUMERICAL PRACTICES IN (DEPENDING ON THE ENTITY OF THE PRACTICE, 1 OR MORE WILL BE CARRIED OUT):\n\n- STELLAR PHYSICS.\n- INTERSTELLAR MEDIUM AND PHYSICS OF GALAXIES\n- EXTRAGALACTIC PHYSICS AND COSMOLOGY\n- OTHER APPLICATIONS." . . "Presential"@en . "FALSE" . . "Large object astrophysics techniques"@en . . "6" . "Specific Competition\nCE1 - Understand the basic conceptual schemes of Astrophysics\nCE7 - Know how to find solutions to specific astrophysical problems by themselves using specific bibliography with minimal supervision. Know how to function independently in a novel research project\nCE10 - Use current scientific instrumentation (both Earth-based and Space-based) and learn about its innovative technologies.\nCE11 - Know how to use current astrophysical instrumentation (both in terrestrial and space observatories) especially that which uses the most innovative technology and know the fundamentals of the technology used\nGeneral Competencies\nCG1 - Know the advanced mathematical and numerical techniques that allow the application of Physics and Astrophysics to the solution of complex problems using simple models\nCG2 - Understand the technologies associated with observation in Astrophysics and instrumentation design\nBasic skills\nCB6 - Possess and understand knowledge that provides a basis or opportunity to be original in the development and/or application of ideas, often in a research context\nCB7 - That students know how to apply the knowledge acquired and their ability to solve problems in new or little-known environments within broader contexts\nCB8 - That students are able to integrate knowledge and face the complexity of formulating judgments based on information that, being incomplete or limited, includes reflections on the social and ethical responsibilities linked to the application of their knowledge and judgments\nCB10 - That students possess the learning skills that allow them to continue studying in a way that will be largely self-directed or autonomous\nExclusive to the Specialty in Observation and Instrumentation\nCX8 - Understand the structure and evolution of nebulae and other large objects\n6. Subject contents\nTheoretical and practical contents of the subject\n- Teachers: Ismael Pérez Fournon (coordinator), Emma Esparza Borges and Fernando Tinaut Ruano. Emma and Fernando will help in the organization and supervision of practices in the observatories and in the reduction and analysis of data in the Student Calculation Center of the Department of Astrophysics.\n\n- Theoretical/practical topics:\n\n1) Main observational techniques in all ranges of the spectrum and astronomical data files.\n\n2) Virtual Observatory.\n\n3) Spectroscopy techniques: multi-object, integral field.\n\n4) Reduction and analysis of astronomical data from CCD image.\n\n5) Practice of photometry of galaxies and transient cosmic sources using the IAC80 telescopes (Teide Observatory, Tenerife), Isaac Newton (Roque de los Muchachos Observatory, La Palma), Las Cumbres Observatory and data from public astronomical archives.\n\n6) Practice of preparing an observation proposal." . . "Presential"@en . "FALSE" . . "Spectropolarimetry in astrophysics"@en . . "6" . "Specific Competition\nCE1 - Understand the basic conceptual schemes of Astrophysics\nCE6 - Understand the structure of matter being able to solve problems related to the interaction between matter and radiation in different energy ranges\nCE7 - Know how to find solutions to specific astrophysical problems by themselves using specific bibliography with minimal supervision. Know how to function independently in a novel research project\nCE9 - Understand the instrumentation used to observe the Universe in the different frequency ranges\nCE10 - Use current scientific instrumentation (both Earth-based and Space-based) and learn about its innovative technologies.\nGeneral Competencies\nCG1 - Know the advanced mathematical and numerical techniques that allow the application of Physics and Astrophysics to the solution of complex problems using simple models\nCG2 - Understand the technologies associated with observation in Astrophysics and instrumentation design\nCG4 - Evaluate the orders of magnitude and develop a clear perception of physically different situations that show analogies allowing the use, to new problems, of synergies and known solutions\nBasic skills\nCB6 - Possess and understand knowledge that provides a basis or opportunity to be original in the development and/or application of ideas, often in a research context\nCB7 - That students know how to apply the knowledge acquired and their ability to solve problems in new or little-known environments within broader contexts\nCB8 - That students are able to integrate knowledge and face the complexity of formulating judgments based on information that, being incomplete or limited, includes reflections on the social and ethical responsibilities linked to the application of their knowledge and judgments\nCB10 - That students possess the learning skills that allow them to continue studying in a way that will be largely self-directed or autonomous\nExclusive to the Theory and Computing Specialty\nCX3 - Understand the origin of polarized radiation and the methods to obtain information about magnetic fields in the Cosmos\n6. Subject contents\nTheoretical and practical contents of the subject\n- Professor: Dr. José Alberto Rubiño Martín\n\n- Topics:\n\n1. INTRODUCTION. Observation of polarized light in astrophysics. Examples: Sun, stars, Milky Way, other galaxies, cosmic microwave background. Review of Maxwell's equations. Description of polarized light. Stokes parameters.\n\n2. SPECTROPOLARIMETERS: Polarimeter prototype. Retarders and polarizers. Jones matrices. Mueller matrices. Examples of devices in optical and radio. Description of systematic errors in real devices.\n\n3. POLARIZATION IN THE CONTINUOUS: Fresnel equations: Reflection and refraction. Expedited charges. Bremsstrahlung. Polarization by scattering Rayleigh, Thomson. Cyclotron and synchrotron radiation. Propagation effects (Faraday rotation). Other effects of astrophysical interest: examples and applications.\n\n- Lecturer: Dr. Tanausú del Pino Alemán\n\n- Lessons:\n\n4. POLARIZATION IN ATOMIC LINES: Quantum model of an atomic transition. Selection rules. Zeeman Broadcast. Strong field and weak field limits. Atomic polarization. Scattering on atomic lines. Statistical equilibrium equations. Hanle effect. Microturbulent case. Applications to solar and stellar magnetism.\n\n5. TRANSPORT OF POLARIZED LIGHT IN STELLAR ATMOSPHERES: Structure of the radiative transport equation for polarized light. Coupling with statistical equilibrium equations. Particular cases. Inference of the thermodynamic and magnetic properties of a stellar atmosphere." . . "Presential"@en . "FALSE" . . "Stellar astrophysics & astronomical techniques"@en . . "5.00" . "The first part of this module is concerned with our understanding of the births, lives and deaths of stars. The starting point is the observational study and classification of stars, arriving at the Hertzsprung-Russell and Mass-Luminosity diagrams. The physics of stars, including the mechanisms by which stars support themselves against gravitational collapse, and how they derive power from nuclear processes and generate elements heavier than Helium, is then examined. The final section of the course is dedicated to astronomical instrumentation where the design of telescopes used in astronomy to detect electromagnetic radiation from radio waves to gamma rays is explored. The module draws on ideas and laws from many different areas of physics and so a reasonable background in physics is expected for students to undertake this course.\n\nLearning Outcomes:\nOn completion of this module students should be able to:\n(1) describe the techniques and results of observations of stars\n(2) derive/calculate information about stars' physical properties from the measurement data\n(3) apply the laws of physics to understand the properties and evolution of stars, and apply models to determine parameters such as central pressure, central temperature, lifetime etc.\n(4) describe the processes of stellar nucleosynthesis\n(5) describe the compact objects that form at the end of stars' lives, including White Dwarf stars, Neutron stars and Pulsars.\n(6) discuss the detection methods and techniques used by astronomical telescopes for operation in different parts of the electromagnetic spectrum, and perform basic calculations of telescope performance and sensitivity\n\nIndicative Module Content:\nRough outline of the course\n\n- Introduction: stellar properties (distances, magnitude, luminosities, etc); The HR diagram; ...\n\n- Stellar structure\n\n- Stellar evolution\n\n- Astronomical techniques: Earth atmosphere; Fundamental concepts; Telescopes" . . "Presential"@en . "FALSE" . . "Theoretical astrophysics"@en . . "5.00" . "Theoretical astrophysics is concerned with the application of the fundamental principles and equations of physics to solve astrophysical problems and to explain astronomical observations. This module covers the theory of radiative processes, astrophysical gas dynamics and an introduction to astrophysical plasmas. Radiative processes includes the equation of radiative transfer and the fundamental theory of radiation fields. The module will then specifically examine bremsstrahlung, synchrotron, Compton, inverse-Compton and line emission mechanisms. Gas dynamics includes basic principles, hydrostatics, waves, shock fronts, accretion, outflows, instabilities and an introduction to plasma physics. These topics will be applied to an extensive range of astronomical problems and observations; including the hot big bang model, aspects of stellar structure and evolution, compact objects, the interstellar medium and high energy astrophysics.\n\nLearning Outcomes:\nOn successful completion of this module a student will (1) understand the principles of astrophysical radiative processes and gas dynamics, (2) understand how fundamental areas of physics combine in different astrophysical settings, (3) solve problems in radiative processes and gas dydnamics and (4) explain select astronomical observations using the tools of theoretical astrophysics." . . "Presential"@en . "FALSE" . . "Data analysis and methods in solar system physics"@en . . "8" . "determination of measurement methods and data analysis. Methods included in the physical description of the solar system are used. Basic methods of space physics and solar physics research, solar observations and evaluation methods, statistic methods, analysis of remote sensing and in situ measurements from space probes, satellites and ground-based observatories, simulation" . . "Presential"@en . "FALSE" . . "General astrophysics I"@en . . "5,0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "General astrophysics II"@en . . "6,0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "Advanced astrophysics"@en . . "20.0" . "#### Prerequisites\n\n* Foundations of Physics 2B (PHYS2591) and Stars and Galaxies (PHYS2621) and Foundations of Physics 3A (PHYS3621).\n\n#### Corequisites\n\n* None.\n\n#### Excluded Combination of Modules\n\n* None.\n\n#### Aims\n\n* This module is designed primarily for students studying Department of Physics or Natural Sciences degree programmes.\n* It builds on the modules Stars and Galaxies (PHYS2621) and Foundations of Physics 3A (PHYS3621) and provides a working knowledge of advanced optical techniques used in modern astronomy and of the radiative processes that generate the emission that is studied in a wide range of astronomical observations at an advanced level appropriate to Level 4 physics students.\n\n#### Content\n\n* The syllabus contains:\n* Astronomical Techniques and Advanced Imaging: Introduction to astronomical techniques, review of optical theory, propagation of light through the atmosphere, adaptive Optics, interferometry, sectroscopy, non-optical techniques.\n* Radiative Processes in Astrophysics: Review of radiative transfer, accelerated charges, Compton processes, synchrotron and Bremsstrahlung, photoionisation/recombination, line formation, abundances, dust, plasma effect, RM and group velocity.\n\n#### Learning Outcomes\n\nSubject-specific Knowledge:\n\n* Having studied this module students will be aware of advanced optical techniques used in modern astronomy, in particular of high angular resolution imaging techniques and their astrophysical applications.\n* They will understand the radiative processes that generate the emission that is studied in a wide range of astronomical observations and will know the observational context of the main theoretical aspects.\n\nSubject-specific Skills:\n\n* In addition to the acqusition of subject knowledge, students will be able to apply knowledge of specialist topics in physics to the solution of advanced problems.\n* They will know how to produce a well-structured solution, with clearly-explained reasoning and appropriate presentation.\n\nKey Skills:\n\n#### Modes of Teaching, Learning and Assessment and how these contribute to the learning outcomes of the module\n\n* Teaching will be by lectures and workshops.\n* The lectures provide the means to give a concise, focused presentation of the subject matter of the module.\n* The lecture material will be explicitly linked to the contents of recommended textbooks for the module, thus making clear where students can begin private study.\n* When appropriate, lectures will also be supported by the distribution of written material, or by information and relevant links online.\n* Regular problem exercises and workshops will give students the chance to develop their theoretical understanding and problem solving skills.\n* Students will be able to obtain further help in their studies by approaching their lecturers, either after lectures or at mutually convenient times.\n* Student performance will be summatively assessed through an open-book examination and formatively assessed through problem exercises.\n* The open-book examination will provide the means for students to demonstrate the acqusition of subject knowledge and the development of their problem- solving skills.\n* The problem exercises provide opportunities for feedback, for students to gauge their progress and for staff to monitor progress throughout the duration of the module.\n\nMore information at: https://apps.dur.ac.uk/faculty.handbook/2023/UG/module/PHYS4161" . . "Presential"@en . "TRUE" . . "Theoretical astrophysics"@en . . "20.0" . "#### Prerequisites\n\n* Foundations of Physics 3A (PHYS3621) and Planets and Cosmology 3 (PHYS3651).\n\n#### Corequisites\n\n* Planets and Cosmology 4 (PHYS4231) if Planets and Cosmology 3 (PHYS3651) has not been taken in Year 3.\n\n#### Excluded Combination of Modules\n\n* General Relativity IV (MATH4051).\n\n#### Aims\n\n* This module is designed primarily for students studying Department of Physics or Natural Sciences degree programmes.\n* It builds on the Level 3 module Foundations of Physics 3A (PHYS3621) and provides an overview of our current understanding of the formation and evolution of cosmic structure and an introduction to Einstein’s general theory of relativity at an advanced level appropriate to Level 4 physics students.\n\n#### Content\n\n* The syllabus contains:\n* Cosmic Structure Formation: Cosmological perturbations, fluid equations, Jeans theory, non-baryonic dark matter, temperature fluctuations in the cosmic microwave background radiation, spherical collapse model, N-body simulations, statistics of galaxy clustering.\n* General Relativity: Gravity as curvature, tensor algebra, mathematics of curved spacetime, the Einstein equations, the Schwarzschild metric, weak field tests of general relativity, black holes.\n\n#### Learning Outcomes\n\nSubject-specific Knowledge:\n\n* Having studied this module students will be able to describe mechanisms that seed small perturbations in the early Universe and will be able to describe mathematically how these perturbations evolve throughout cosmic history. They will understand the physical processes that have shaped our universe.\n* They will be aware of the principles of general relativity, including the interpretation of gravity as spacetime curvature, and be able to apply them to the simplest gravitational systems.\n\nSubject-specific Skills:\n\n* In addition to the acqusition of subject knowledge, students will be able to apply knowledge of specialist topics in physics to the solution of advanced problems.\n* They will know how to produce a well-structured solution, with clearly-explained reasoning and appropriate presentation.\n\nKey Skills:\n\n#### Modes of Teaching, Learning and Assessment and how these contribute to the learning outcomes of the module\n\n* Teaching will be by lectures and workshops.\n* The lectures provide the means to give a concise, focused presentation of the subject matter of the module.\n* The lecture material will be explicitly linked to the contents of recommended textbooks for the module, thus making clear where students can begin private study.\n* When appropriate, lectures will also be supported by the distribution of written material, or by information and relevant links online.\n* Regular problem exercises and workshops will give students the chance to develop their theoretical understanding and problem solving skills.\n* Students will be able to obtain further help in their studies by approaching their lecturers, either after lectures or at mutually convenient times.\n* Student performance will be summatively assessed through an open-book examination and formatively assessed through problem exercises.\n* The open-book examination will provide the means for students to demonstrate the acqusition of subject knowledge and the development of their problem- solving skills.\n* The problem exercises provide opportunities for feedback, for students to gauge their progress and for staff to monitor progress throughout the duration of the module.\n\nMore information at: https://apps.dur.ac.uk/faculty.handbook/2023/UG/module/PHYS4201" . . "Presential"@en . "TRUE" . . "The sun and the heliosphere"@en . . "6.0" . "### Teaching language\n\nEnglish\n\n### Objectives\n\nCourse that presents the main phenomena of solar activity, introduces magnetohydrodynamics (MHD) for the description of plasmas in astrophysics and provides some examples of its application to the Sun. Describes the heliosphere and presents some models for its description. Introduces and explores the concept of space weather.\n\n### Learning outcomes and competences\n\n1- To distinguish between the active and the quiet sun and to identify the main solar active phenomena associated with its magnetic field\n\n2- To use magnetohydrodynamics (MHD) as a theory to describe the behaviour of plasmas in the presence of magnetic fields\n\n3- To obtain MHD solutions for static fields and for waves in plasmas\n\n4- To use MHD in order to model the equilibrium in arcades/prominences, the energy release in solar flares via magnetic reconnection, the heating of the solar corona and the acceleration of the solar wind\n\n5- To describe the heliosphere and its main properties recognize its importance for the space weather\n\n### Working method\n\nPresencial\n\n### Program\n\n1\\. The Sun \n\\- Observations of the Sun. Solar activity. \n\\- Photosphere, transition region, chromosphere and corona. \n\\- Structure and configuration of the solar magnetic field \n \n2. The magnetohydrodynamic (MHD) description \n\\- Properties and fundamental equations \n\\- Equilibrium solutions \n\\- Waves in MHD \n \n3. Applications of MHD to the Sun \n\\- Equilibrium models for sunspots, arcades and prominences \n\\- Magnetic reconnection and solar flares. \n\\- Models for heating the solar corona. \n\\- The solar wind. models \n \n4\\. The heliosphere. \n\\- Origin and exploration \n\\- The global magnetic field of the heliosphere \n\\- Space weather \n\n### Mandatory literature\n\nEric Priest; Magnetohydrodynamics of the Sun, Cambridge University Press, 2014. ISBN: 0521854717 \nE. R. Priest; Solar Magnetohydrodynamics, Reidel Publishing Company, 2000. ISBN: 9027721386 \n\n### Complementary Bibliography\n\nAndre´ Balogh, Louis J. Lanzerotti, Steven T. Suess; The Heliosphere through the Solar Activity Cycle, Springer, 2008. ISBN: 978-3-540-74301-9 \nF. Shu; The Physics of Astrophysics. Volume 2: Gas Dynamicss, University Science Book, 1992. ISBN: 0935702652 \nL. Golub, Jay M. Pasachoff; The solar corona, Cambridge University Press, 1997. ISBN: 0521485355 \nMari Paz Miralles, Jorge Sánchez Almeida; The Sun, the Solar Wind, and the Heliosphere, Springer, 2011. ISBN: 978-90-481-9786-6 \nH. Zirin; Astrophysics of the Sun, Cambridge University Press, 1988. ISBN: 0521316073 \nMarkus J Aschwanden; Physics of the Solar Corona. An Introduction with Problems and Solutions, Springer, 2005. ISBN: 3-540-30765-6 \n\n### Teaching methods and learning activities\n\nExpository method intercalated by problem solving. Some problems will be given to students in order to be solved in classes or at home. \n \nPresentation of an article in a short talk and report, from a list provided at the beginning of the semester\n\n### keywords\n\nPhysical sciences > Astronomy > Astrophysics \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nexam: 75,00\nWritten assignment: 25,00%\n\n**Total:**: 100,00% \n\n### Amount of time allocated to each course unit\n\nAutonomous study: 120,00 hours\nFrequency of lectures: 42,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nThe student has frequency to the course if he/she misses no more than 1/4 of the planned theoretical-practical classes (TP's).\n\n### Calculation formula of final grade\n\nDistributed evaluation:\n\nFinal Mark = 25% of Mark of the Mini Test + 25% of Mark of the Talk presenting the paper and its critical analysis + 50% of Mark of the Test (to take place in 1st exam season). \n \nMinimum mark in Test: 7/20. \n \nThe Final Mark will be the mark of the normal (1st) season.\n\nIf the student has not passed, he can use the 2nd season exam for this purpose. In this case, the exam will be used as an alternative to the mini test and test components, corresponding only to 75% of the final grade. \n \nThe students with a special status, namely working-students will be subject to an evaluation equal to the remaining students. \n\n### Classification improvement\n\nIt is not allowed to improved grades on the Report/Talk presenting the paper. An improvement in the components of the Mini Test and Test is possible through an exam which counts only for 75% of the final grade.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=508145" . . "Presential"@en . "TRUE" . . "Extragalactic astrophysics and galaxy formation"@en . . "6.0" . "Learning objectives\n\nReferring to knowledge\n\nThe main objective of the course is to provide students with an updated overview of the structure and dynamics of galaxies, their formation in a cosmological context and the physical mechanisms that contribute to the evolution of their spectrophotometric, chemical, dynamic and morphological characteristics. The course covers both the observational properties of galaxies and related objects in different redshifts and the modelling of processes involved in their formation and evolution.\n\n \n\nReferring to abilities, skills\n\n— Gain the capacity for critical analysis and synthesis regarding explanations and models associated with the subject area of the course.\n\n— Gain reflection capacity and creativity relating to assignments set in class or proposed by students within the subject area of the course.\n\n— Become familiar with data acquisition and analysis techniques used in astrophysics.\n\n \n\n \n\nTeaching blocks\n\n \n\n1. Preliminary aspects\n1.1. Useful units and equations\n\n1.2. Relations between apparent and intrinsic astronomical quantities\n\n2. Introduction to galaxies\n2.1. What is a galaxy?\n\n2.2. Types of galaxies\n\n2.3. Modern classification of galaxies\n\n2.4. Bivariate distributions of galactic parameters\n\n2.5. Luminosity function: generalities\n\n2.6. Luminosity function and stellar mass function for red and blue galaxy populations\n\n2.7. Physical origin of the luminosity function\n\n2.8. Formation of stars\n\n3. Active galactic nucleus (AGN)\n3.1. Operative definition\n\n3.2. Structure of the basic physiology of supermassive black holes\n\n3.3. AGN taxonomy\n\n3.4. Physics of accretion\n\n3.5. Formation of supermassive black holes\n\n4. Late-type galaxies (LTG)\n4.1. Basic structural characteristics\n\n4.2. Atomic and molecular gas content\n\n4.3. Dust content\n\n4.4. Metallicity\n\n4.5. Scaling laws\n\n4.6. Results of ALFALFA mapping\n\n5. Early-type galaxy (ETG)\n5.1. Basic structural characteristics\n\n5.2. Light profiles\n\n5.3. Kinematics\n\n5.4. Gas and dust content\n\n5.5. Metallicity\n\n5.6. Scaling laws\n\n6. Galaxy groups and evolution\n6.1. Main characteristics of galaxy clusters\n\n6.2. Dynamic models of viralised systems\n\n6.3. Scaling laws in galaxy clusters\n\n6.4. Environmental dependence of galaxy properties\n\n6.5. Evolutionary effects of galaxy aggregation\n\n6.6. Environment-dependent evolutionary mechanisms\n\n6.7. Pre-processing\n\n6.8. Observational examples of galaxy interactions\n\n7. Structure formation in the universe\n7.1. Large-scale structure of the universe\n\n7.2. Structure formation and cosmology\n\n8. Cosmological density perturbations: linear evolution\n8.1. Basic equations\n\n8.2. Fluids without pressure\n\n8.3. Fluids with pressure: Jeans scale\n\n9. Spherical collapse\n9.1. Perturbation energy\n\n9.2. Movement of a spherical layer\n\n9.3. Maximum expansion and collapse\n\n9.4. Spherical collapse limits\n\n10. Relaxation time scales and processes\n10.1. Binary interactions\n\n10.2. Dynamic friction\n\n10.3. Violent relaxation\n\n11. Dark matter halos\n11.1. Statistics based on the linear field of density perturbations\n\n11.2. Press-Schechter formalism\n\n11.3. Excursion set formalism\n\n11.4. Peak theory\n\n11.5. Internal structure of halos: density, velocity dispersion and anisotropy\n\n12. Formation and evolution of galaxies\n12.1. Hierarchical formation of galaxies\n\n12.2. Analytical and semianalytical models\n\n12.3. Modelling of dark matter: grouping of halos and internal structure\n\n12.4. Baryon physics: gas cooling, formation of stars, feedback processes\n\n12.5. Growth of supermassive black holes and emission of AGN\n\n12.6. Population III stars\n\n12.7. Galactic structure: discs and bulges\n\n12.8. Interactions between galaxies and the environment\n\n13. High-z universe\n13.1. High-z galaxies: Lyman-break galaxies, Lyman-alpha emitters, ULIRG\n\n13.2. Evolution with z of global properties of galaxies and the intergalactic environment\n\n14. Introduction to galaxy formation simulations and large-scale structure\n14.1. Theoretical models of galaxy formation\n\n14.2. N-body simulations\n\n14.3. Hydrodynamic simulation\n\n14.4. Examples of simulations\n\n \n\n \n\nTeaching methods and general organization\n\n \n\nThe course consists of lectures with the support of audiovisual material. Some renowned specialists in the field may give some supervised computer practical classes, within the hours of face-to-face teaching. Students are also expected to participate by raising and debating questions on the topics explained in class, under teacher supervision.\n\n \n\n \n\nOfficial assessment of learning outcomes\n\n \n\nContinuous assessment considers the following aspects:\n\n— Showing the knowledge acquired through a project on the analysis of a galaxy cluster, carried out and presented in small groups, (70%) and the delivering of specific tasks (30%).\n\n— The attitude and level demonstrated by students when they ask and discuss questions in ordinary classes or in the time allocated for this purpose.\n\n \n\nExamination-based assessment\n\nSingle assessment consists of a multiple-choice examination on the whole content of the course.\n\nRepeat assessment is held in early September and consists of an examination similar to the one held in June.\n\n \n\n \n\nReading and study resources\n\nCheck availability in Cercabib\n\nBook\n\nH. Mo, S.D.M. White & F. van den Bosch. Galaxy formation and evolution. Cambridge University Press, 2010 Enllaç\n\n\nLongair, M. S. Galaxy formation. 2nd ed. Berlin : Springer, cop. 2008\n\n Enllaç\n\nBinney, James ; Tremaine, Scott. Galactic dynamics. 2nd ed. Princeton : Princeton University Press, 2008 Enllaç\n\n\nSparke, Linda S. ; Gallagher, John S. Galaxies in the universe : an introduction. 2nd ed. Cambridge : Cambridge University Press, 2007 Enllaç\n\n1a ed. Enllaç\n\nSpinrad, Hyron. Galaxy formation and evolution. Berlin [etc.] : Springer ; Chichester : Praxis, cop. 2005 Enllaç\n\n\nColes, Peter ; Lucchin, Francesco. Cosmology : the origin and evolution of cosmic structure. 2nd ed. Chichester : John Wiley, cop. 2002 Enllaç\n\n\nArticle\n\nR.S. Somerville & R. Davé Physical models of galaxy formation in a cosmological framework. Dins Annu. Re. Astron. Astrophys. 53:51-113 (2015)\n\n\nKruit, Pieter C. van der ; Freeman, Ken C. Galaxy disks. Dins: Annu. Re. Astron. Astrophys. 49 :301-371 (2011) Enllaç\n\n\nBenson, A. J. Galaxy formation theory. Dins: Physics Reports. 495 : 33-86 (2010) Enllaç\n\n\nBaugh, C. M. A primer on hierarchical galaxy formation.: the semi-analytical approach. Dins: Reports on progress in physics. 69 : 3101-3156 (2006) Enllaç\n\n\nWeb page\n\nWhittle ASTR 5630 & 5640 Graduate extragalactic astronomy Enllaç\n\n\nElectronic text\n\nKruit, Pieter C. van der. Structure and dynamics of galaxies. 2011 Enllaç\n\n\nPhilipps, Steve. Galaxies. 2009 Enllaç\n\n\nAvila-Reese, V. Understanding galaxy formation and evolution. 2006\n\nMore information at: http://grad.ub.edu/grad3/plae/AccesInformePDInfes?curs=2023&assig=568432&ens=M0D0B&recurs=pladocent&n2=1&idioma=ENG" . . "Presential"@en . "FALSE" . . "High energy astrophysics"@en . . "3.0" . "Learning objectives\n\nReferring to knowledge\n\nThe objective of this course is to acquire research training in high-energy astrophysics, from an observational and theoretical point of view. The subjects provides students with basic and updated knowledge to properly prepare them for the subsequent career in research. For those who do not foresee a career in research, the learning gained on this master’s degree will boost their skills and increase their experience, which could be useful in the job market.\n\nTo understand the high-energy universe in which we live, first we explain physical mechanisms that can accelerate particles to high energies and radiation processes that lead to astrophysical sources. Then, we study the phenomenology of various kinds of astrophysical high-energy sources, such as supermassive black holes in galactic nuclei, X-ray binary stars, pulsars or supernova remnants. The most recent observational results are presented and the implication is discussed in the available models.\n\nHigh-energy astrophysics is currently in a golden age due to the results that are being obtained from existing observatories, which represent a unique opportunity to advance in the field of high energies. The following observatories are notable:\n— Soft X-ray satellites, such as XMM-Newton or Chandra.\n— Hard X-ray satellites, such as INTEGRAL or Swift.\n— High-energy gamma-ray satellites, such as Fermi.\n— Cherenkov telescopes, such as MAGIC, HESS or VERITAS.\n— Neutrino detectors, such as IceCube.\n\nThe enormous amount of information that has been gathered by these instruments over years requires professionals to process the data properly and contribute to advances in the physics field.\n\n \n\n \n\nTeaching blocks\n\n \n\n1. 0. Introduction - Messengers from space\n* Cosmic rays\n\n Neutrinos\n\n Gravitational waves\n\n Electromagnetic waves \n\n2. 1. Particle acceleration and radiation mechanisms in high energy astrophysics\n* 1.1. Particle acceleration mechanisms\n\n 1.2. Diffusion\n\n 1.3. Energy losses\n\n 1.3. Radiative processes\n\n 1.3.1. Thermal emission\n\n 1.3.2. Synchrotron radiation\n\n 1.3.3. Inverse Compton scattering\n\n 1.3.4. Bremsstrahlung\n\n 1.3.5. Hadronic processes\n\n 1.3.6. Particle annihilation\n\n3. 2. Accretion and ejection in relativistic sources\n* 2.1. Accretion onto compact objects \n\n 2.2. Outflows: jets and winds (general physical description)\n\n 2.3. Flow dynamics (production, propagation, content, termination)\n\n 2.4. Emission in relativistic outflows: electron-positron pairs \n\n 2.5. Emission in relativistic outflows: protons and nuclei \n\n 2.6. Radiation reprocessing\n\n4. 3. Phenomenology of accreting sources with outflows\n* 3.1. Observational tools (analysis and fundamental diagrams)\n\n 3.2. X-ray binary accretion modes\n\n 3.3. Disks and jets \n\n 3.4. Black holes at all scales: from X-ray binaries to AGNs\n\n5. 4. High-energy gamma-ray sources in the Universe\n* 4.1. High-energy gamma-ray detectors and satellites\n\n 4.2. Imaging atmospheric Cherenkov telescopes\n\n 4.3. Galactic high-energy gamma-ray sources (pulsars, pulsar wind nebulae, supernova remnants, X-ray and gamma-ray binaries, etc.)\n\n 4.4. Extragalactic high-energy gamma-ray sources (AGNs, GRBs, EBL, etc.)\n\n 4.5. Fundamental physics at high-energy gamma rays (dark matter, Lorentz invariance, etc.)\n\n \n\n \n\nTeaching methods and general organization\n\n \n\nLecturers explain the topics in the programme with the support of audiovisual material and the Internet among others.\nStudents are given the material presented in each class in electronic format.\nStudents must submit an assignment and give an oral presentation, and a written synthesis test to prove the comprehension of the knowledge acquired.\n\n \n\n \n\nOfficial assessment of learning outcomes\n\n \n\nStudents should work on a topic of high energy astrophysics proposed by teachers. The work, which must be presented orally and submitted in writing, allows part of the assessment to be carried out. The assessment is completed with a written synthesis test and taking into account active participation in class. The percentage of the grade for each part is:\n- Participation: 20%\n\n- Written synthesis test: 30%\n\n- Written work: 20%\n\n- Oral presentation of the work: 30%\n\nThe same system is used for re-evaluation as for evaluation.\n\n \n\n \n\nReading and study resources\n\nCheck availability in Cercabib\n\nBook\n\nAharonian, F. A. Very high energy cosmic gamma radiation : crucial window on the extreme universe. Singapore : World Scientific Publishing, cop. 2004. Enllaç\n\n\nCharles, Philip A. ; Seward, Frederick D. Exploring the X-ray universe. Cambridge : Cambridge University Press, 1995. Enllaç\n\n\nLongair, M. S. High energy astrophysics. 3rd ed. Cambridge : Cambridge University Press, 2011 Enllaç\n\n\nPacholczyk, A. G. Radioastrofísica : procesos no térmicos en fuentes galácticas y extragalácticas. Barcelona : Reverté, DL 1979 Enllaç\n\n\nRomero, Gustavo E. ; Paredes i Poy, Josep Maria. Introducción a la astrofísica relativista. Barcelona : Publicacions i Edicions Universitat de Barcelona, cop. 2011 Textos docents ; 365\n\n\nMore information at: http://grad.ub.edu/grad3/plae/AccesInformePDInfes?curs=2023&assig=568433&ens=M0D0B&recurs=pladocent&n2=1&idioma=ENG" . . "Presential"@en . "FALSE" . . "Astrophysics and cosmology"@en . . "6.0" . "http://grad.ub.edu/grad3/plae/AccesInformePDInfes?curs=2023&assig=569104&ens=M0D0G&recurs=pladocent&n2=1&idioma=ENG" . . "Presential"@en . "FALSE" . . "Astrophysics from space"@en . . "4.0" . "This course is taught at the UGent\n\nPosition of the course: \nAstrophysics is one of the cornerstones of the scientific programmes of the various space organizations. This course presents the various astrophysics space programs, the most important astrophysics space missions and the scientific highlights from space astrophysics in the different wavelength regions\n\nContents\n\nIntroduction \n* Optical astronomy: overview and missions \n* Optical astronomy: scientific highlights (extragalactic distance scale, Hubble Deep Field, supermassive black holes, stellar evolution) \n* Infrared astronomy: overview and missions \n* Infrared astronomy: scientific highlights (starburst galaxies, CMB, star and planet formation) \n* Radio astronomy from space \n* High energy astronomy: overview and missions \n* High energy astronomy: scientific highlights (X-ray background radiation, galaxy clusters, X\n* ray binaries, gamma ray bursts)\n\nInitial competences\nThis course can only be followed by students who have registered for the Master of Space Studies.\n\nFinal competences\n\n1  Know the most important players in space and the astrophysics part of their science program. \n2  Discuss the necessity, advantages and disadvantages of astrophysics from space in the various wavelength regions. \n3  Describe the main innovations and properties of the most important astrophysics space missions. \n4  Discuss the scientific highlights of astrophysics from space in the frame of the different space missions\n\nMore information at: https://studiekiezer.ugent.be/studiefiche/en/C002851/2023" . . "Presential"@en . "FALSE" . . "Astrophysics"@en . . "8" . "Interstellar Medium and Star Formation" . . "Presential"@en . "TRUE" . . "Astrophysics II"@en . . "8" . "no data" . . "Presential"@en . "TRUE" . . "Physical concepts in astronomy"@en . . "8" . "no data" . . "Presential"@en . "TRUE" . . "Theoretical astrophysics"@en . . "7" . "no data" . . "Presential"@en . "TRUE" .