. "Physics"@en . . "Computer Science"@en . . "Astronomy"@en . . "English"@en . . "Seminar in particle physics and astrophysical sciences"@en . . "5" . "LEARNING OUTCOMES\nDevelop your oral (“presentation”) and peer review (“feedback”) skills, develop your ability to promote your expertise and market yourself, help with the MSc thesis project.\n\nCONTENT\nMSc thesis plan, MSc thesis disposition, career development related tasks, oral presentation and being opponent to other students’ presentations." . . "Presential"@en . "TRUE" . . "Msc maturity test"@en . . "0" . "LEARNING OUTCOMES and CONTENT are not available" . . "Presential"@en . "TRUE" . . "Cosmology II"@en . . "5" . "LEARNING OUTCOMES\nYou will learn to calculate the primordial perturbations produced by a given inflation model.\nYou will understand how these primordial perturbations develop into the present large-scale structure of the universe.\nYou will understand how these perturbations affect the anisotropy of the cosmic microwave background and how the latter can be used to determine the values of the cosmological parameters.\nCONTENT\nCosmological inflation in the early universe as explanation for the initial conditions of the Big Bang\nInflation models and how inflation generates primordial perturbations (density fluctuation sand gravitational waves)\nStructure formation: how primordial perturbations develop into the present large-scale structure: Newtonian first-order perturbation theory; a little bit of relativistic perturbation theory\nCosmic microwave background anisotropy; its description and physics; connection to primordial perturbations and cosmological parameters" . . "Presential"@en . "TRUE" . . "Introduction to particle physics I"@en . . "5" . "LEARNING OUTCOMES\nAim of the course is to familiarize students to the basic concepts of modern particle physics and learn the most fundamental calculational techniques. This will lay the foundation for more in-depth studies of Quantum Chromodynamics, Electroweak theory and Higgs physics in follow-up courses.\n\nCONTENT\nUnderlying concepts [special relativity, quantum mechanics]\nDecay rates and cross sections [Lorentz-invariance, matrix element]\nThe Dirac equation [relativistic QM => spin + antimatter]\nInteraction by particle exchange [Feynman diagrams]\nElectron-positron annihilation [calculations in perturbation theory]\nElectron-proton elastic scattering [form factor]" . . "Presential"@en . "TRUE" . . "Introduction to particle physics II"@en . . "5" . "LEARNING OUTCOMES\nThe course covers the structure of the Standard Model, quantum chromodynamics, electroweak interactions, neutrino-oscillations, the Higgs mechanism.\n\nThe emphasis is on calculations with tree-level Feynman diagrams.\n\nCONTENT\nquantum chromodynamics\nV-A -structure of weak interactions\nweak interactions of leptons\nneutrino oscillations\nweak interactions of quarks and CP violation\nW and Z bosons, and tests of the Standard Model\nHiggs Mechanism" . . "Presential"@en . "TRUE" . . "Quantum mechanics IIa"@en . . "5" . "LEARNING OUTCOMES\nThe student knows the formalism on non-relativistic quantum mechanics. The student can apply perturbation theory and other approximation methods to time-dependent perturbations and scattering problems in atomic, nuclear and condensed matter physics. The student understands the assumptions underlying different approximations and can estimate the range of validity of different approximation methods within the considered context. The student can couple three angular momenta, knows spherical tensor operators and can apply Wigner-Eckart theorem.\n\nCONTENT\nTime dependent perturbation theory, Fermi's Golden rule, sudden and adiabatic approximations.\nScattering theory: construction of Lippmann-Schwinger equation and its solution in Born approximation.\nScattering theory: partial wave method for spherically symmetric potentials, scattering resonances.\nCoupling of angular momenta, spherical tensor operators and Wingner-Eckart theorem.\nPath integral formulation of quantum mechanics" . . "Presential"@en . "FALSE" . . "Quantum mechanics IIb"@en . . "5" . "LEARNING OUTCOMES\nThe student knows the methods of second quantisation in non-relativistic many-body quantum mechanics and can apply these. The student can quantize free boson and fermion fields. The student can quantize electromagnetic field and apply the theory to describe interaction of quantised matter and radiation.\n\nCONTENT\nMany-particle methods in non-relativistic quantum mechanics\nElements of quantum field theory.\nQuantum theory of radiation." . . "Presential"@en . "FALSE" . . "Mathematical methods of physics a"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will be familiar with basic concepts of group theory, group representation theory, and topology. The student can identify different common groups, study if their representations are reducible, irreducible or not, and knows why the theory of groups and their unitary representations is important in quantum physics of systems with various symmetries. The student also understands distinctions between nonhomeomorphic topological spaces and understands the use of topological invariants (such as homotopy groups) in their classification.\n\nCONTENT\nGroup theory: finite groups, continous groups, conjugacy classes, cosets, quotient groups\n\nRepresentation theory of groups: complex vector spaces and representations, symmetry tranformations in quantum mechanics, reducible and irreducible representations, characters\n\nTopology: topological spaces, topological invariants, homotopy, homotopy groups" . . "Presential"@en . "FALSE" . . "Mathematical methods of physics b"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will be familiar with basic concepts of calculus on differentiable manifolds and Riemannian geometry, which are mathematical tools used in physics e.g. in the contexts of general relativity and gauge field theories. The student will also be familiar with basics of Lie algebra representation theory, which is used e.g. in particle physics and condensed matter theory. The student can work with differential forms, express metrics in different coordinates and compute metric tensors of general relativity. He also understands basic representations of Lie algebras used e.g. in the theory of strong interactions.\n\nCONTENT\nDifferentiable manifolds and calculus on manifolds: differentiable manifolds, manifolds with boundary, differentiable maps, vector fields, 1-form fields, tensor fields, differentiable map and pullback, flow generated by a vector field, Lie derivative, differential forms, Stokes' theorem\n\nRiemannian geometry: metric tensor, induced metric, connections, parallel transport, geodesics, curvature and torsion, covariant derivative, isometries, Killing vector fields\n\nSemisimple Lie algebras and representation theory: SU(2), roots and weights, SU(3), introduction to their most common unitary irreducible representations" . . "Presential"@en . "FALSE" . . "Gaseous radiation detectors and scintillators"@en . . "5" . "LEARNING OUTCOMES\nKnowledge of radiation detectors and its principle of operation\nTreatment of the signals\nAnalysis of its performance\nCONTENT\nIntroduction of the interaction of radiation with matter; this include the processes undergo by a particle traversing a block of matter and its energy loses mechanism. The particles in study are: photons, light charged particles, heavy charged particles and neutrons. Then study of Scintillation mechanism and generation of light by energy deposition in a crystal. This will include the conversion of photons light flash into an electrical signal. Finally similar study will be done for gas-filled detectors and detailed study of detectors developed in house for CERN experiments" . . "Presential"@en . "FALSE" . . "Semiconductor radiation detectors"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will…\n\nknow the basics of the interaction of radiation and matter;\nbe familiar with the application of detectors in the studies of particle, X-ray, gamma-ray and neutron radiation;\nknow the operational principle of semiconductor diode detectors and other selected types of solid-state detectors;\nhave an idea of the principles of detector signal processing and data-acquisition;\nbe familiar with the application of radiation detectors in the instrumentation of nuclear and particle physics.\nCONTENT\n1. Interaction of radiation with matter.\n\n2. Solid-state detectors.\n\n3. Detector read-out." . . "Presential"@en . "FALSE" . . "Physics of positrons in solids and defects"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will be able\n\nto describe sources of positrons and the interactions between energetic positrons and matter\nto explain the positron-electron annihilation process by using fundamental laws of physics\nto explain the working principles of energy, time and angle-resolved gamma spectroscopy of positron annihilation processes\nto derive the relationships between fundamental annihilation parameters detected in experiments\nto analyze experimental data from the perspective of defects in solids\nto discuss the use of theoretical calculations of positron annihilation signals in identification of defects in solids\nto study the scientific literature on positron annihilation in detail\nCONTENT\nPhysics of positrons in solids. Defect spectroscopy with positron annihilation." . . "Presential"@en . "FALSE" . . "Physics of semiconductor devices"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will…\n\nUnderstand the significance of semiconductor devices in modern society;\nUnderstand the physical grounds of the operation of semiconductor devices: Understand the meaning of atomic bonds, crystal structure, crystal defects, energy bands, electrical defect states, charge carriers, charge carrier transport, optical properties, recombination, Fermi distribution, donors, acceptors, mobility, lifetime, drift and diffusion, and resistivity in semiconductor material.\nUnderstand the concepts of heterostructures, nanostructures and graphene in semiconductor devices;\nUnderstands and is able to explain the operational principle of semiconductor pn-diode;\nUnderstand the principle of Light-to-Electricity conversion and can explain the operational principles of photoconductors, photodiodes and solar cells;\nUnderstand the principle of Electricity-to- Light conversion and can explain the operational principles of scintillators, LEDs and Lasers;\nUnderstand the principle of transistors and can explain the operational principles of bipolar transistor and MOSFET;\nUnderstand the principles of semiconductor processing;\nCONTENT\n1. Physics behind the operation of semiconductor devices,\n\n2. Operational principles of various semiconductor devices." . . "Presential"@en . "FALSE" . . "Laboratory course on instrumentation"@en . . "no data" . "LEARNING OUTCOMES\nAfter the laboratory course the student will be able to:\n\nwork in a scientific laboratory environment taking into account strict safety rules such as caution for high-voltages, gases, chemicals, delicate instruments, and radiation safety,\nknow the physics of radiation detectors (introductory level),\nconstruct a gas-filled radiation detector starting from simple everyday materials such as aluminum beverage can and nuts and bolts,\noperate radiation detectors and data acquisition systems using typical laboratory equipment, such as source-meter-unit, radiation sources, gas piping, preamplifier, linear amplifier, multi-channel analyzer, and oscilloscope,\nwrite scientifically high quality laboratory reports.\nCONTENT\nLaboratory exercises will provide the students with hands-on & minds-on training about working in laboratory environment and about radiation detector technologies. The work will include gas detectors and detector read-out systems." . . "no data"@en . "FALSE" . . "Particle physics phenomenology"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will...\n\nlearn to know relativistic kinematics and the Standard model of particle physics.\nbe able to apply relativistic kinematics to calculation of total and differential cross-sections/widths.\nunderstand more deeply the Standard model of particle physics and its basis.\nbe able to apply the understanding of the Standard model to particle physics phenomenology especially at the Large Hadron Collider (LHC).\nbe familiar with the most popular extension of the Standard Model of particle physics.\nCONTENT\nRelativistic kinematics: special relativity, phase space, two-, three- and multi-particle final states.\n\nStandard Model: theoretical framework, principle of gauge invariance, quantum electrodynamics (QED) and chromodynamics (QCD), elektroweak unification, the Higgs mechanism and electroweak precision measurements.\nBeyond the Standard Model (BSM): signs of BSM physics, basic principles of extensions of the Standard Model, Grand Unified Theories, supersymmetric and extra dimensional models.\nHadron colliders: deep inelastic scattering and hadron-hadron interactions.\nLHC phenomenology: QCD, electroweak, top and Higgs" . . "Presential"@en . "FALSE" . . "Particle physics experiments"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will...\n\nlearn the basic principles of particle accelerators and their applications in other fields.\nunderstand the dynamics of particles in an accelerator.\nbe able to apply the understanding to design a particle accelerator.\nlearn the basic principles of particle detectors of high energy physics and their applications in other fields.\nunderstand the different types of particle detectors and their strengths and weaknesses as well as the synergy between them.\nbe able to apply the understanding to design a high energy physics experiment.\nCONTENT\nAccelerators: Particle Accelerator History and Basics, Transverse Beam Dynamics and Accelerator Lattice, Longitudinal Beam Dynamics, Accelerating Cavities, Electron Dynamics, Imperfections & instabilities, Colliders & cooling, The Large Hadron Collider (LHC), Future colliders and accelerator applications.\n\nExperiments: Particle Detector History and Basics, Tracking and Particle Interaction with Matter, Gaseous charged particle detectors, Semiconductor charged particle detectors, Scintillation and Photon Detectors, Energy Measurement, Jet Reconstruction and Particle Flow, Calorimeters, Trigger and Data Acquisition, Detector Systems, The LHC experiments." . . "Presential"@en . "FALSE" . . "Computing methods in high energy physics"@en . . "5" . "LEARNING OUTCOMES\nYou will learn tools used in the data/physics analysis in a typical High Energy Physics experiment.\n\nCONTENT\nThe course provides an introduction to learning to use software used in a typical High Energy Physics experiment. The CMS experiment is used as an example.\n\nTopics covered include:\n\nShort review of UNIX\nC++\nROOT\nCombining languages\nCross section and branching ratio calculations\nEvent generators\nDetector simulations\nReconstruction\nFast simulation\nGrid computing" . . "Presential"@en . "FALSE" . . "Statistical methods"@en . . "5" . "LEARNING OUTCOMES\nAfter the course, the student will...\n\nlearn to know the basics of statistics and statistical distribution as well as being able to apply the correct distribution.\nunderstand hypotheses testing and different methods for hypotheses testing as well as the strengths and weaknesses of the methods.\nunderstand parameter estimation based on maximum likelihood and least squares methods as well as the strengths and weaknesses of the methods.\nbeing able to apply methods of hypothesis testing and parameter estimation as well as make the correct statistical interpretation.\nbeing familiar with confidence intervals and unfolding.\nCONTENT\nFundamental concepts: experimental errors and their correct interpretation, frequentist & Bayesian interpretation of probability, the most common statistical distributions and their applications.\nMonte Carlo methods: basics of Monte Carlo methods and generation of an arbitrary distribution.\nHypothesis testing: the concept of hypothesis testing, a test statistic, discriminant multivariate analysis, goodness-of-fit tests and ANOVA.\nParameter & error estimation: the concept of parameter estimation, an estimator, the maximum likelihood method and the method of least squares.\nConfidence intervals & Unfolding." . . "Presential"@en . "FALSE" . . "Basics of monte carlo simulations"@en . . "5" . "LEARNING OUTCOMES\nAfter completion the course you will be able:\n\nGenerate uniform and non-uniform random numbers by using different methods\nApply pseudo- and quasirandom numbers for different tasks\nPerform Monte Carlo integration of multidimensional functions\nEstimate the statistical error of the mean for different methods\nGenerate the synthetic data to improve on estimation of the average and the error of the mean\nImprove the convergence of the Monte Carlo integration result using different methods\nCreate your own Game of life by using the Cellular automata principle" . . "Presential"@en . "FALSE" . . "Introduction to machine learning"@en . . "5" . "Description and learning outcomes are not available." . . "Presential"@en . "FALSE" . . "Quantum field theory I"@en . . "5" . "LEARNING OUTCOMES\nThe student knows basics of relativistic quantum field theory and can apply the methodology to leading order scattering processes.\n\nCONTENT\nClassical field theory and quantization of free real and complex scalar fields.\n\nQuantization of free Dirac field.\n\nInteracting theories and development of perturbation theory. \n\nExamples in quantum electrodynamics.\n\nIntroduction to renormalisation." . . "Presential"@en . "FALSE" . . "Quantum field theory II"@en . . "5" . "LEARNING OUTCOMES\nThe student knows path integral formulation of quantum mechanics and field theory. The student can apply path integral methods to quantise abelian gauge theory. The student knows the need of renormalisation in quantum field theory.\n\nCONTENT\nPath integral formulation of quantum field theory.\n\nGrassmann variables and path integral for fermion fields.\n\nGenerating functionals\n\nGauge theory and its quantization\n\nRenormalisation of scalar field theory." . . "Presential"@en . "FALSE" . . "Quantum field theory III"@en . . "5" . "CONTENT\nSystematics of renormalization\n\nRenormalization group\n\nQuantization of Yang-Mills theory, BRST invariance\n\nRenormaliation of Yang-Mills theory, asymptotic freedom." . . "Presential"@en . "FALSE" . . "Quantum field theory Iv"@en . . "5" . "CONTENT\nSpontaneous symmetry breaking \n\nEffective potential in quantum field theory\n\nHiggs mechanism\n\nRenormalization of the electroweak theory\n\nAnomalies." . . "Presential"@en . "FALSE" . . "Theories beyond the standard model"@en . . "no data" . "Description and learning outcomes are not available." . . "no data"@en . "FALSE" . . "Introduction to the physics of neutrinos"@en . . "5" . "LEARNING OUTCOMES\n \n\nCONTENT\nNeutrinos in the Standard Model, neutrino mass terms (Dirac and Majorana, seesaw mechanism), neutrino mixing, oscillations of neutrinos in vacuum, neutrinos in matter (oscillations in matter with constant density and adiabatic conversion)." . . "Presential"@en . "FALSE" . . "Path integral quantization of gauge field theories"@en . . "5" . "CONTENT\nBrief introduction to path integral as solution of diffusion equation. Path integrals in quantum mechanics. Quantization of systems with constraints. Path integrals in quantum field theory; generating functional; Schwinger action principle. Grassmann variables and path integrals for fermionic fields. Path integral quantization in QED. Path integral quantization of non-Abelian gauge field theories; Faddeev-Popov ghosts. Symmetries in functional formalism; Ward-Takahashi identities." . . "Presential"@en . "FALSE" . . "General relativity I"@en . . "5" . "LEARNING OUTCOMES\nYou will learn the physical and mathematical structure of the theory of general relativity.\n\nYou will learn how to do calculations in general relativity, including how to find the precession of the orbit of Mercury and the bending of light by the Sun.\n\nCONTENT\nChapter 1: review of symmetries in Newtonian mechanics, review of special relativity from the spacetime point of view, relativity principle in Newtonian mechanics and special relativity, electrodynamics in special relativity\n\nChapter 2: the equivalence principle, manifolds, tensors, the metric\n\nChapter 3: covariant derivative and connection, parallel transport, geodesics, curvature, Riemann tensor\n\nChapter 4: Einstein equation, Newtonian limit\n\nChapter 5: The Schwarzschild solution, precession of the perihelion of Mercury, bending of light by the Sun" . . "Presential"@en . "FALSE" . . "General relativity II"@en . . "5" . "LEARNING OUTCOMES\nYou will learn the physical and mathematical structure of the theory of general relativity.\n\nYou will learn how to do calculations in general relativity, including with black holes, linear perturbation theory, gravitational waves and a little bit also in cosmology.\n\nCONTENT\nChapter 1: action formulation of general relativity\n\nChapter 2: global structure of the Schwarzschild solution, black holes, Penrose diagram, brief overview of charged and rotating black holes and Hawking radiation\n\nChapter 3: perturbation theory around Minkowski space, gauge transformations, gravitomagnetism, gravitational waves, generation of gravitational waves by a binary system, energy loss due to emission of gravitational waves\n\nChapter 4: Killing vectors, symmetric spacetimes, FLRW spacetime, de Sitter space, anti-de Sitter space, Penrose diagrams" . . "Presential"@en . "FALSE" . . "Galaxy survey cosmology"@en . . "5" . "CONTENT\nLarge scale galaxy surveys are the main observational tools to advance cosmology during the coming decade. These surveys determine the three-dimensional distribution of galaxies in the universe and, by measuring distortions of galaxy images due to gravitational lensing, map also the distribution of dark matter. From these distributions and their statistical measures, including 2- and 3-point correlation functions, power spectra and bispectra, the large-scale properties of the universe can be determined. One key question is the nature of dark energy, the cause for the accelerated expansion of the universe. It can be probed by measuring accurately the expansion history of the universe and the gravity-driven growth of large-scale structure. These galaxy surveys include the Dark Energy Survey (DES) and the future space missions Euclid and Roman. Finland (Universities of Helsinki, Turku, Jyväskylä, Oulu, and Aalto University) participates in Euclid. The course PAP352 Galaxy Survey Cosmology focuses on the distribution of galaxies and the course PAP353 Gravitational Lensing on gravitational lensing, especially on weak lensing (shear) surveys." . . "Presential"@en . "FALSE" . . "Gravitational lensing"@en . . "5" . "LEARNING OUTCOMES\nThe course gives you the theoretical basis to understand gravitational lensing as a physical phenomenon. You will understand the relation between lensing theory and observations, and how lensing can be used to extract cosmological information. You will have the conceptual basis that allows you to deepen your knowledge by reading further literature or publications.\n\nCONTENT\nGravitational lensing is a powerful cosmological probe. This course is an introduction to the theory of gravitational lensing in the context of cosmology. The theory is built on the theory of general relativity, and on the FRW model of the universe. The focus is on cosmology, thus we will mainly be working at the weak-lensing limit, strong lensing is touched only briefly.\n\nThe course is motivated by Euclid, the European Space Agency’s satellite mission to probe the large scale structure and expansion history of the universe. The course forms a natural continuation to the course of Galaxy Survey Cosmology, but can also be taken individually.\n\nContents:\n\n- Propagation of light in general relativity\n\n- Lensing geometry and basic concepts\n\n- Weak and strong lensing\n\n- Magnification and distortion\n\n- Relation to observations\n\n- Lensing as a cosmological probe\n\n- Shear field, E- and B-modes\n\n- Lensing spectrum and correlation function\n\n- Shear as a spin-2 field" . . "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" . . "Statistical inverse methods"@en . . "5" . "LEARNING OUTCOMES\nYou will learn\n\nAdvanced statistical methods to describe and analyze research data\nTheory and practice of statistical estimation and testing\nMultivariate methods\nMonte Carlo statistical techniques\nBayesian inference\nStatistical inversion using Markov Chain Monte Carlo methods\nCONTENT\nStatistical inference, linear model, nonlinear model, kernel estimation, multivariate methods, Bayesian inference, Monte Carlo methods, MCMC." . . "Presential"@en . "TRUE" . . "Plasma physics"@en . . "5" . "LEARNING OUTCOMES\nYou will obtain solid knowledge of basic concepts and phenomena of plasma physics, useful for further studies concerning laboratory, fusion, space and astrophysical plasmas.\nYou will obtain skills to analytically solve basic problems related to plasma physics, such as particle drifts in simple magnetic field and electric field configurations\nYou will obtain skills to derive various basic plasma equations starting from basic set of fluid and Maxwell equations\nYou will obtain solid conceptual understanding and theory behind several key basic plasma phenomena, such as magnetic reconnection, magnetohydrodynamic stability and plasma instabilities.\nYou will obtain a good understanding of different approaches in plasma physics (single particle, kinetic and fluid)\nCONTENT\nAfter a brief introduction and a short review of electrodynamics needed in plasma physics, the following topics are discussed: motion of charged particles in electromagnetic fields, collisions and plasma conductivity, kinetic plasma description, macroscopic plasma quantities and equations, magnetohydrodynamics (MHD), magnetic reconnection, MHD waves, cold plasma waves, warm plasma, plasma physics and fusion research." . . "Presential"@en . "TRUE" . . "Advanced course in observational astronomy I"@en . . "5" . "LEARNING OUTCOMES\nParticipants of the course will learn about preparation, conduction and data reduction of modern astronomical observations. They will participate in the forefront research projects on stellar evolution, galaxy evolution and cosmology and contribute to obtaining the new measurements.\n\nCONTENT\nThe students will be performing observations with Nordic Optical Telescope (NOT) and reduce the data they obtain. The course covers instrumentation, visibility studies, observational conditions and planning the observational run; Telescope control system; Preparation of the observing run: choosing exposures, filters, grisms for the science goals; Calibration observations; Target acquisition; Performance spectroscopic and imaging observations; Data reduction and visualization; Performing the scientific experiment: planing, conducting, adjusting, reporting. The students will be given a short introduction to the data reduction, with a full detail on data reduction being a subject of PAP308 course." . . "Presential"@en . "FALSE" . . "Advanced course in observational astronomy II"@en . . "5" . "LEARNING OUTCOMES\nAfter completing the course the students should be able to: (1) Identify and extract raw data together with the corresponding calibration frames from the ESO Science Archive that are relevant to the astrophysical science question being studied; (2) Reduce these data using a relevant pipeline provided by ESO (use e.g. high-resolution UVES and near-infrared ISAAC spectroscopic data as examples); (3) Carry out an analysis of complex spectroscopic data; (4) Carry out photometry in fully-reduced astronomical imaging observations including both relative photometry and absolute photometry with the full photometric calibration; (5) Carry out both absolute and relative astrometry in fully-reduced astronomical imaging observations; (6) Carry out automatic source detection, characterization and photometry in astronomical imaging observations; (7) Produce a written course report\n\nCONTENT\nThe course is organized in cooperation with the Finnish Centre for Astronomy with ESO (FINCA). The course includes teaching in the form of lectures and supervised hands-on work on the data. The lectures cover the use of the ESO Science Archive and ESO data reductions pipelines (e.g. reduction and analysis of high-resolution optical spectroscopic and near-infrared spectroscopic data), the common methods for photometry and astrometry, automatic source extraction and characterization in astronomical images. The course presents the tools astronomers currently use to analyze large numbers of complex spectroscopic data in AGN (active galactic nuclei) and star-forming galaxies and how users can apply these tools for analysis to their own (potentially non-AGN/galaxy related) data. The course will also help students scale the sometimes daunting initial learning curve by connecting them with the tool's designers or expert users. The students are expected to work individually on their datasets and write-up their individual course reports at the end of the course." . . "Presential"@en . "FALSE" . . "Special course in observational astronomy"@en . . "5" . "LEARNING OUTCOMES\nThe students will learn how to reduce their data obtained in Advanced Observational Astronomy course I.\n\nThe students will learn the general principles of modern astronomical data reduction.\n\nCONTENT\nReduction of astronomical images and spectra using IRAF tasks. The course offers the required software skills to successfully perform the data reduction on the scientific projects of PAP306. Lectures cover the IRAF tasks that the students need to reduce the data from NOT, and provide training using example data" . . "Presential"@en . "FALSE" . . "Interstellar matter"@en . . "5" . "LEARNING OUTCOMES\nYou will know the chemical and physical composition of the interstellar medium (ISM), in both its gas and dust components. You will understand the principles that determine the physical state of the ISM and the general stability of interstellar clouds. You will learn the main steps of the star-formation process, starting with molecular cloud cores and ending up in the formation of protostars. You will understand how the process is affected by the physical conditions within the interstellar clouds and how each stage of the process can be investigated with observations at optical, infrared, and radio wavelengths.\n\nCONTENT\nThe course covers the properties and physical processes in the interstellar medium (ISM), especially in connection with star formation. The course starts with a general description of the structure, evolution, and properties of the ISM, with an emphasis on dense molecular clouds. We will then study the interplay of gravity, turbulence, and magnetic fields that leads to the formation of dense cores within the molecular clouds and, as a result of their collapse, to the formation of new stars. The gravitational and thermal balance and the chemical evolution of the ISM along the star-formation process will also be examined. The course ends with a discussion of the observable properties of young stellar objects." . . "Presential"@en . "FALSE" . . "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" . . "Time series analysis in astronomy"@en . . "5" . "LEARNING OUTCOMES\nThe students will learn the theory, the application and the programming of different period finding methods that can be used to analyse astronomical data.\n\nCONTENT\nThe following methods are taught: the Discrete Chi Square Methods, the power spectrum method and other statistical methods. All these will be programmed and applied to real data" . . "Presential"@en . "FALSE" . . "Variable stars"@en . . "5" . "LEARNING OUTCOMES\nPreviously unpublished photometry of a chromospherically active star is analysed with different period analysis methods. Detailed modelling of the light curves is performed. The following phenomena are studied: activity cycles, active longitudes and differential rotation. Basic scientific writing and reading is practiced, as well as the use of references and databases. The aim is to report the results in a refereed paper, where the authors will be all the students that pass the course. The best student will be the main author.\n\nCONTENT\nStudying the presence of activity cycles, active longitudes and differential rotation in real unpublished photometric data. Learning basic scientific writing, reading and use of references, as well as databases. The aim is to report the results in a refereed paper, where the authors will be all the students that pass the course. The best student will be the main author." . . "Presential"@en . "FALSE" . . "Stellar magnetic activity"@en . . "5" . "LEARNING OUTCOMES\nAfter the course the student will have a basic understanding of the physical processes behind stellar magnetic activity and different approaches of modelling, e.g. mean field magnetohydrodynamics and direct numerical simulations. The student will also be familiar with observational methods used for research in this field. The student will know how stellar rotation and the convective turnover time influences the activity, and why these change during the stellar evolution. The aim is also, that the students are aware of the open questions in this research, and that this may inspire them for further studies.\n\nCONTENT\nStellar magnetic activity is an advanced course in stellar astrophysics. The course gives a basic understanding of the physics behind solar and stellar magnetic activity, e.g. spots, flares, chromospheric activity and coronal mass ejections. Another major focus of the course is on observations, in particular imaging methods based on optical photometry, spectroscopy and spectropolarimetry." . . "Presential"@en . "FALSE" . . "Introduction to light scattering"@en . . "5" . "LEARNING OUTCOMES\nElectromagnetic Scattering and Absorption\" is the first advanced course on elastic electromagnetic scattering by arbitrary objects (usually called particles). As compared to the wavelength, the sizes of the objects can be small or large, or of the order of the wavelength. As to the shape of the objects, the main emphasis is on spherical particles and, subsequently, on the so-called Mie scattering. The optical properties of the objects are typically described by the refractive index. During the course, the student will become familiar with the concepts of electromagnetic scattering and will learn how to use existing computer codes in astronomical and atmospheric applications.\n\nCONTENT\nIntroduction to light scattering (electromagnetic scattering) is the first advanced course on elastic light scattering by arbitrary objects (usually called particles). As compared to the wavelength, the sizes of the objects can be small or large, or of the same order. As to the shape of the objects, the main emphasis is on spherical particles and, consequently, on Mie scattering. The optical properties of the objects are typically described by the refractive index. During the course, the student becomes familiar with the concepts of light scattering, learns how to use existing computer codes in astronomical and atmospheric applications, and completes a hands-on computer programming project (for example, involving ray tracing)." . . "Presential"@en . "FALSE" . . "Computational light scattering"@en . . "5" . "LEARNING OUTCOMES\nThe course Electromagnetic Scattering I offers an introduction and theoretical foundation for elastic electromagnetic scattering by arbitrary objects (usually called particles). As compared to the wavelength, the sizes of the objects can be small or large, or of the order of the wavelength. As to the shape of the objects, main emphasis is on spherical particles and, subsequently, on the so-called Mie scattering. The optical properties of the objects are typically described by the refractive index.\n\nCONTENT\nComputational light scattering assesses elastic light scattering (electromagnetic scattering) by particles of arbitrary sizes, shapes, and optical properties. Particular attention is paid to advanced computational methods for both single and multiple scattering, that is, to methods for isolated particles and extended media of particles (cf. dust particles in cometary comae and particulate media on asteroids). Theoretical foundations are described for the physics of light scattering based on the Maxwell equations and for a number of computational methods. In single scattering, the methods include, for example, the volume integral equation, discrete-dipole approximation, T-matrix or transition matrix, and finite-difference time-domain methods. In multiple scattering, the methods are typically based on Monte Carlo ray tracing. These include far-field radiative transfer and coherent backscattering methods and their extensions incorporating full-wave interactions. Students are engaged in developing numerical methods for specific scattering problems. The development and computations take place in both laptop and supercomputing environments." . . "Presential"@en . "FALSE" . . "Astrophysical light scattering problems"@en . . "5" . "LEARNING OUTCOMES\nThe course Electromagnetic Scattering II offers an introduction and theoretical foundation for elastic electromagnetic scattering by complex random media of particles, in other words, for multiple electromagnetic scattring. As compared to the wavelength, the media can span from a few wavelengths onwards to the scale of thousands of wavelengths. As to the geometry of the media, media composed of both spherical and nonspherical particles are treated. Finally, the course includes practical application of existing multiple-scattering software in both laptop and supercomputing environments to interpret spectroscopic, photometric, and polarimetric observations in astronomy as well as scattering measurements in the laboratory.\n\nCONTENT\nAstrophysical light scattering problems provides a cross-scale journey in light scattering (electromagnetic scattering) with a particular emphasis in applications. The course starts with an introduction to the basic concepts and computational methods, whereafter experimental measurements are assessed. Various applications are introduced for planetary system objects, interstellar and circumstellar dust, and exoplanets. Students are actively engaged in the interpretation of spectroscopic, photometric, and polarimetric observations as well as laboratory measurements. The interpretation takes place using both laptop and supercomputing environments." . . "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" . . "Galaxy formation and evolution"@en . . "5" . "LEARNING OUTCOMES\nThe student will learn to understand galaxy formation as process. The student will learn to solve practical problems in observational cosmology. The student will\nmaster Newtonian perturbation theory required to explain the origin of galaxies. The student will understand the role of dark matter in galaxy formation. The student\nwill learn how the initial perturbation spectrum developed to the observed distribution of galaxies. The student will be able to describe the non-linear evolution of\ndensity perturbations using simple analytic models. The student will learn the dominant cooling processes relevant for galaxy formation and understand the importance\nof star formation and supernova feedback for galaxy evolution. The student will learn the properties and formation scenarios of disk galaxies, elliptical galaxies and\nactive galaxies. The student will learn to the importance of galaxy interactions and encounters as a force shaping the evolution of galaxies.\n\nCONTENT\nBasic elements of galaxy formation. The classification of galaxies. Statistical properties of the galaxy population. Galaxies at high redshifts. Robertson-Walker metric and the Friedmann equations.\nThe evolution of small perturbations. The Jeans' instability in a static and expanding Medium. Cosmological horizons and perturbations on superhorizon scales. Adiabatic and isothermal perturbations. Hot and cold dark matter in galaxy formation models. The two-point correlation function for galaxies. The initial power spectrum and transfer functions. The non-linear collapse of density perturbations. Top-hat collapse and the Zeldovich approximation. The Press-Schechter mass function and dark matter density profiles. The cooling and heating of gas in dark matter haloes. The cooling function and galaxy formation. Molecular clouds and self-regulated star formation. Supernova feedback: The ejection and heating of gas. Formation of disk galaxies and the origin of disk scaling relations. Galaxy interactions and encounters. Tidal stripping and dynamical friction. Orbital decay and galaxy merging. Structure and formation of elliptical galaxies. The physics of Active galaxies (AGNs). The formation and evolution of AGNs." . . "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" . . "Radiative transfer"@en . . "5" . "LEARNING OUTCOMES\nYou will learn how the microphysical properties of the medium (gas and dust) are linked to the macroscopic radiative transport of energy.\nYou will understand the common approximations (such as local thermodynamic equilibrium or the large-velocity-gradient approximation) that are used to analyse astronomical observations of radiation.\nYou will know the common implementation principles of the programs that are used in detailed astronomical radiative-transfer modelling.\nYou will able to use existing radiative-transfer programs to model observations of dust continuum (extinction, scattering, and emission) and spectral-line radiation.\nCONTENT\nThe course covers the use of radiative transfer methods in the modelling of astrophysical sources. We will start by examining how the micro-physical properties of the medium - gas and dust - are linked to the interactions with radiation. We will then examine some common approximations used in numerical radiative transfer before studying the more exact radiative transfer modelling, especially with Monte Carlo simulations. The course includes practical work with radiative transfer software and (as part of report work) possibly even the writing of a simple radiative transfer program of one's own. The topics include: radiative transfer equation; local thermodynamic equilibrium (LTE); escape-probability formalism and the large velocity gradient (LVG) approximation; radiative transfer calculations for dust continuum; radiative transfer calculations for line emission; Monte Carlo radiative transfer methods; radiative transfer on parallel machines and GPUs; software for radiative transfer modelling." . . "Presential"@en . "FALSE" . . "Space applications of plasma physics"@en . . "5" . "LEARNING OUTCOMES\nYou will obtain solid understanding of space physics, giving a good background in further studies and research in space plasma physics\nKnowledge of basic solar physics, e.g., the structure of the Sun, and how energy is generated and transferred\nYou will obtain solid theoretical knowledge behind several key phenomena in space plasma physics, such as solar wind and interplanetary magnetic field, collisionless shocks, magnetospheric, and ionospheric physics\nYou will obtain skills to analyse some key data sets related to course topics (such as magnetospheric physics behind the auroral displays)\nYou will obtain solid physics-based understanding on how the solar structures affect the near-Earth dynamics, leading to space weather phenomena\nCONTENT\nThe course contains an introduction to most important topics in space plasma physics: the Sun, solar wind, formation of the magnetosphere, ionosphere, magnetospheric dynamics, solar wind/magnetosphere-ionosphere coupling, magnetospheres of other planets, and astrophysical plasmas." . . "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" . . "Advanced space plasma physics"@en . . "10" . "LEARNING OUTCOMES\nAfter completing this course, you are intended to have the ability to:\n\nnavigate the terminology and idiosyncrasies of space physics publications, enabling you\nto independently study and learn from research papers in the field\nderive different mathematical approaches to plasma physics from first principles, most\nimportantly: single-particle, kinetic and magnetohydrodynamic equations\ndiscern which of these approaches are applicable and practical for a given physical\nproblem\nobtain satellite measurement data from public data sources and interpret their results\nanalyze plasma wave properties for remote sensing of plasma conditions\nidentify and appraise plasma phenomena at the Sun, in the solar wind, in Earth's\nmagnetosphere and in the ionosphere\nindependently approach and study new plasma physics problems, and communicate\nyour findings\nCONTENT\nThese lectures are intended to advanced undergraduate and post-graduate students interested in space physics, plasma physics, applications of electrodynamics, statistical physics, hydrodynamics, etc. The course starts with plasma fundamentals, reviewing the basic concepts and looks more in depth to plasma distribution functions. The other topics include\n\nA detailed description of charged particle motion in electromagnetic fields, including time and spatially varying fields, including adiabatic invariants, motion in current sheets, and galactic cosmic rays will be covered.\nThe wave propagation in dielectric media, the main focus being on propagation through the layered ionosphere, but cold plasma wave theory will be briefly revised.\nA detailed coverage of the Vlasov theory and Landau damping\nA brief revision of magnetohydrodynamic (MHD) theory, the main focus will be put on subjects like force-free fields, flux ropes in space plasmas and magnetic helicity.\nPlasma Instabilities (micro- and macroinstabilities)\nTheory of collisionless shocks waves, dissipation of shocks, shock acceleration and solar energetic particles\nMagnetic reconnection (both theory and observations in space plasmas)\nBasics of solar dynamo\nRadiation and scattering (e.g., Bremsstrahlung, cyclotron and synchrotron)\nTransport (Fokker-Planck theory)\nThe contents of the course are oriented around the research fields that are investigated in the Space Physics research group. The course stays close to the possible thesis topics and concepts that actual research work in the field is based on." . . "Presential"@en . "FALSE" . . "Numerical methods in scientific computing"@en . . "10" . "LEARNING OUTCOMES\nYou will learn to know the most common numerical methods and algorithms\nYou will understand the strenghts and weaknesses of these algorithms\nYou will be able to apply these algorithms using\nself-made programs\nnumerical libraries\nnumerical programs.\nCONTENT\nTools, computing environment in Kumpula, visualization\nBasics of numerics: floating point numbers, error sources\nLinear algebra: equations, decompositions, eigenvalue problems\nNonlinear equations: bisection, secant, Newton\nInterpolation: polynomes, splines, Bezier curves\nNumerical integration: trapeziodal, Romberg, Gauss\nFunction minimization: Newton, conjugate gradient, stochastic methods\nGeneration of random numbers: linear congruential, shift register, non-uniform random numbers\nStatistical description of data: probability distributions, comparison of data sets\nModeling of data: linear and nonlinear fitting\nFourier and wavelet transformations: fast Fourier transform, discreet wavelet transform, applications\nDifferential equations: ordinary and partial differential equations" . . "Presential"@en . "FALSE" . . "Numerical space physics"@en . . "5" . "LEARNING OUTCOMES\nYou will learn about the various simulation methods that are used in space physics, why they are used and how they are used, and what their strengths and weaknesses are.\n\nYou will learn hands-on what running a simulation entails and how the data can be analysed.\n\nYou will understand the principles behind the numerical methods of the simulations, in particular magnetohydrodynamics.\n\nYou will be able to study space physics problems using advanced numerical simulations.\n\nCONTENT\nThe course consists of three thematic packages.\n\nTo begin with, the role of simulation methods in space physics is reviewed in which the how, what and why of simulations are presented on a general level. More focused topics such as methods for visualisation and analysis of simulation data are also discussed.\nThe second theme focuses on individual algorithms, in particular the numerical methods of hyperbolic conservation laws, magnetohydrodynamics, and PIC simulations.\nA major part of the course is the final hands-on project assignment in which the students individually apply a simulation method to study a particular problem in space physics." . . "Presential"@en . "FALSE" . . "Master's programme in Particle Physics and Astrophysical Sciences"@en . . "https://www.helsinki.fi/en/degree-programmes/particle-physics-and-astrophysical-sciences-masters-programme" . "120"^^ . "Presential"@en . "What are the laws of nature governing the universe from elementary particles to the development of the solar system, stars, and galaxies? In the Master’s Programme in Particle Physics and Astrophysical Sciences, you will focus on gaining a quantitative understanding of these phenomena.\n\nWith the expertise in basic research that you will gain in the programme, you might pursue a career in research. You will also acquire proficiency in the use of mathematical methods, IT tools and/or experimental equipment, as well as strong problem-solving and logical deduction skills. These will qualify you for a wide range of positions in the private sector.\n\nAfter completing the programme, you will:\n\n-Have wide-ranging knowledge of particle physical and/or astrophysical phenomena.\n-Have good analytical and computational skills and the ability to make sophisticated deductions.\n-Be able to apply theoretical, computational and/or experimental methods to the analysis and understanding of various phenomena.\n-Be able to apply your knowledge of particle physical and astrophysical phenomena as well as identify their interconnections.\n-Be able to formulate hypotheses and test them based your knowledge"@en . . . . "2"@en . "FALSE" . . . "Master"@en . "Thesis" . "no tuition, other costs may apply" . "Euro"@en . "15000.00" . "None" . "A Master’s degree in elementary particle physics or astrophysical sciences provides you with excellent qualifications for postgraduate education in research or for a career in diverse positions both in Finland and abroad. As a Master’s graduate you could begin a career in research and development in industry as well as in universities and other research institutes that enable you to conduct independent research on a topic that interests you."@en . "2"^^ . "TRUE" . "Upstream"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Finnish"@en . . "Faculty of Science"@en . .