. "Stellar Physics"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Stellar structure and evolution"@en . . "6" . "the student can formulate the basic laws of physics and apply them to describe the stellar\nstructure.\nthe student can formulate nuclear physics processes that take place in stellar\ninteriors.\nthe student can formulate the various equations-of-state of relevance for\nstellar interiors.\nthe student can formulate all the important phases of the life cycle for stars of\nvarious mass.\nthe students can formulate the end products of stellar evolution as a function\nof the birth mass.\nthe students can use the modern state-of-the-art open-access computercode MESA to compute\nstellar models and to interpret the interior profiles of all the physical quantities of relevance for stellar interiors." . . "Presential"@en . "TRUE" . . "Stellar structure and evolution"@en . . "6" . "Stellar observations and the quest for understanding stars have always been at the core of astronomy since ancient times. Stars are not only extraordinary physics laboratories, but they are also vital to our understanding of the life cycle of systems at all scales, such as planets, galaxies and the intergalactic medium. In this course, you will first learn the basic physics of stellar structure in all relevant physical regimes. Then, we will follow a journey through a star’s life where its structure changes as a function of time. We will only focus on isolated stars.\n\nOutcome:\nAfter completion of this course, you will be able to answer quantitative and qualitative questions about a star’s interior structure and life path, when considering an isolated star, ignoring magnetic fields and rotation.\r\n\r\nThis means that after this course you will be able to:\r\n\r\nRun and process the output of the MESA stellar evolution code\r\nRecognise a star’s evolution stage from its observational appearance\r\nName the main uncertainties in the current knowledge of stellar structure and evolution\r\nWrite a clear and professional scientific report" . . "Presential"@en . "TRUE" . . "Stellar structure and evolution"@en . . "6" . "Stellar observations and the quest for understanding stars have always been at the core of astronomy since ancient times. Stars are not only extraordinary physics laboratories, but they are also vital to our understanding of the life cycle of systems at all scales, such as planets, galaxies and the intergalactic medium. In this course, you will first learn the basic physics of stellar structure in all relevant physical regimes. Then, we will follow a journey through a star’s life where its structure changes as a function of time. We will only focus on isolated stars\n\nOutcome:\nAfter completion of this course, you will be able to answer quantitative and qualitative questions about a star’s interior structure and life path, when considering an isolated star, ignoring magnetic fields and rotation.\r\n\r\nThis means that after this course you will be able to:\r\n\r\nRun and process the output of the MESA stellar evolution code\r\n\r\nRecognise a star’s evolution stage from its observational appearance\r\n\r\nName the main uncertainties in the current knowledge of stellar structure and evolution\r\n\r\nWrite a clear and professional scientific report" . . "Presential"@en . "TRUE" . . "Binary stars"@en . . "6" . "- explain the importance of binaries in the context of the determination\nof basic stellar parameters\n- derive the orbital elements of binary stars\n- understand and explain the role of binarity in the chemical properties of some binaries\n- outline the role of compact binaries as test laboratories of general relativity" . . "Presential"@en . "TRUE" . . "Star formation"@en . . "6" . "• To identify the conditions for star formation\n• To become acquainted with the basic ingredients of the star formation process\n• To understand the dynamical processes within disks\n• To situate our solar system in the broad context of planet formation" . . "Presential"@en . "TRUE" . . "Stellar atmospheres and stellar winds"@en . . "6" . "• The student can understand the main processes involved in radiation transfer\n• The student can interpret analytical and numerical solutions of radiation transfer, as described in the scientific literature, and can compare these methods with the ones illustrated in the course\n• The student can interpret the spectra of stellar atmospheres in function of temperature, gravity and chemical composition of the star\n• The student can understand the different physical causes for the onset of a stellar wind\n• The student can interpret observations of stellar winds using basic physical concepts, illustrated by means of simplified analytical equations or complex theoretical computer models" . . "Presential"@en . "TRUE" . . "Variable stars"@en . . "3" . "Definition of variability. Physical and geometrical variable stars. Pulsating and chemically peculiar stars. T Tauri stars Solar-type variability, pulsars. Binary stars (visual, spectroscopic, eclipsing, polarimetric). Roche model of close binary stars. Proximity effects in close binaries. Rossiter McLaughlin rotational effect. Mass loss and transfer. Secular effects (apsidal motion, circularization and synchronization of the orbit) Symbiotic stars. Cataclysmic variables. Supernovae. Mass accretion and accretion disks. Evolution of binary stars. Observational techniques of the stellar astronomy (photometry, spectroscopy, polarimetry, interferometry). Introduction to the photometric and spectroscopic data reduction. Time-series analysis, period analysis and the method of (O-C) diagrams.\n\nOutcome:\nGet acquainted with essential knowledge of variable stars classification and methods of their observations." . . "Presential"@en . "FALSE" . . "How to build a startup company"@en . . "3" . "Learners gain practical, hands-on experience and knowledge about ideation, idea selection, assess their business potential, test their hypothesis in practice and develop appropriate business model. Formed teams gain understanding on entrepreneurship environment, communicate with potential users/clients and build prototypes. Workshops are integrated with individual work and practical tasks, which enable learners to develop their product/service, define value proposition, revenue model and marketing approach. The programme requires commitment, willigness to cooperate, learn teamwork, presentation skills, cope with challenges and stress associated with start-up founding and reflect learning experience.\r\nTeams get guidance from experienced start-up founders and mentors. The programme ends with business ideas presentation at Kaleidoskoop pre-selection from where TOP10 get to pitch at sTARTUp Day .\r\nTeams are enocuraged to execute their projects or business ideas and/or become founders.\n\nOutcome:\nSuccesful learner:\r\n- has gained knowledge about idea development process from ideation to idea selection, value proposal and business model\r\n- is able to test hypotheses related to execution and develop ideas (product/service) in accordance with customer needs,\r\n- is able to assess and analyze the potential market need,\r\n- has gained teamwork skills,\r\n- is able to present business or project idea to potential investors." . . "Hybrid"@en . "TRUE" . . "Asteroseismology"@en . . "6" . "• interpret modern data of non-radially oscillating stars\n• apply time series analysis and mode identification techniques\n• work out research results within a small team of students\n• summarize research results in a written report and talk\n• summarize highlights of selected international papers in asteroseismology" . . "Presential"@en . "TRUE" . . "Binary stars"@en . . "6" . "no data" . . "Presential"@en . "FALSE" . . "Star formation"@en . . "6" . "no data" . . "Presential"@en . "FALSE" . . "Stellar atmospheres and stellar winds"@en . . "6" . "no data" . . "Presential"@en . "FALSE" . . "Asteroseismology"@en . . "6" . "no 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" . . "Late stages of stars, supernovae and gamma-ray bursts"@en . . "7,6" . "This course addresses the late stages of stellar evolution, with focus on the massive stars which end their lives\nas supernovae and/or gamma ray bursts. The theory and stages of nuclear burning from helium ignition to the\nformation of an iron core are laid out, and the origin the elements in the periodic table is discussed. The\nimportant role of neutrino cooling for the now more rapid and qualitatively different stellar evolution is\nemphasized. The connection between stellar properties, such as mass and metallicity, and observational\nclassifications are discussed in the context of the supernova that results.\nThe course further treats the physics of supernova explosions, and how advanced computer simulations have\nimproved our understanding of these. We review the fundamental processes forming the light curve and\nspectra of the supernova, and diagnostic methods to determine the structure of the ejecta. Results from theory\nand observations are combined to describe the landscape of successful explosions versus failed ones leading\nto black hole formation, and associations between different stellar classes and supernova types.\nGamma ray bursts are reviewed, and the connection of these to the most massive and rapidly rotating stars in\nthe Universe is discussed. We study also briefly exotic transients such as superluminous supernovae and\nkilonovae. Learnining outcomes: - describe the star's late evolutionary stages, both on microphysical and macrocopic scales, as\nwell as the connection between stellar properties and observational classes.\n- use publicly available software to make simulations of a star’s evolution, and analyse how\nchanged assumptions affect the evolution.\n- account for the different phases in a supernova explosion, observational properties of supernovae, and\nclassifications based on these properties.\n- deduce and apply analytic formulae to estimate the physical parameters of a supernova from observed light\ncurves and spectra.\n- describe fundamental phenomenology of gamma-ray bursts, models for their emission processes, and\nrelation to the central engine.\n- couple together results from observations, simulations, and theory to differentiate between well established\nand more speculative properties of massive stars, supernovae, and gamma ray bursts.\n- argue for the origin of each element in the periodic table." . . "Presential"@en . "TRUE" . . "Advanced projects in stellar evolution"@en . . "5" . "Description of qualifications\nThe aim of the course is allow in-depth advanced projects and specialisation with a topic linked directly to the lecture course on Advanced Stellar Evolution and the project course in Stellar Evolution. The course will be an extension of the course on the projects in Stellar Evolution and it is a requirement that the student follow the projects course before starting on the advanced project course. The Advanced projects course is non-obligatory for students that follow the Advanced Stellar Evolution lecture course, but the aim is to coordinate the teaching and content of the Advanced Stellar Evolution lecture course and the Stellar Evolution projects with the advanced projects in Stellar Evolution. The course will start in the semester following the Advanced Stellar Evolution lecture course. The course on advanced projects in Stellar Evolution will allow more extended projects than the course on projects in Stellar Evolution.\n\nWhen the course is finished the student is expected to be able to:\n\nPlan and execute an advanced project with a theoretical or practical focus.\nAnalyse data or perform modelling or simulations.\nSearch for relevant scientific literature.\nEvaluate the results and boundary conditions for a specific research project\nCollaborate in smaller groups with the aim of producing a scientific result\nPresent the results as a small talk at a final workshop day.\nContents\nThe course is closely linked to the lecture course on Advanced Stellar Evolution and the course on projects in Stellar Evolution and will focus on in-depth advanced study and specialisation within research on Stellar Evolution. Both theoretical and practical projects are offered. Examples: Advanced modelling, simulations, advanced data analysis, littérature studies. The specific possible advanced projects will be introduced at the start of the course. The advanced project is performed in small groups and under supervision - Support from other staff (incl. postdocs, phd-students, guests, etc.)." . . "Presential"@en . "FALSE" . . "Advanced stellar evolution"@en . . "10" . "Description of qualifications\nThe aim of the course is to provide a detailed background for stellar structure and evolution. Focus is on theoretical as well as observational aspects of stellar evolution. \n\n  \n\nThe learning outcomes of the course are: \n\n  \n\nDescribe the basic physical principles determining the structure and evolution of a star. \nAccount for the most important phases in the evolution of stars, for all relevant stellar masses. \nAccount for the circumstances where the simple description is inadequate. \nDiscuss relevant physical aspects during the extreme phases of stellar evolution. \nEvaluate which aspects of the physical description of stellar evolution that in particular causes uncertainties in the modelling. \nCarry out simple derivations of relevant equations for stellar structure. \nDescribe the observational evidence for the different stages of stellar evolution. \nDiscuss and describe observations of stars relevant for stellar structure – specifically with focus on asteroseismology. \nPerform simple analysis of time series data with focus on extraction of stellar oscillation frequencies. \nFind relevant scientific information, e.g., in the original scientific literature, and evaluate and use this information in a written report related to the scientific content of the evaluation project. \nContents\nAfter a brief summary of the basic description of stellar structure, including a more detailed presentation of important aspects of the physics of stellar interiors and an introduction to stellar hydrodynamics, the different evolution stages of stars are presented through a combination of numerical results and simplified analysis. In addition we discuss some aspects of stellar pulsations, explosive stages of stellar evolution, including supernova explosions. An important part of this course we will contain a discussion of observations of stars as well as data analysis with focus on astroseismology and how this can be used to test models of stellar structure and evolution. The exercise classes will include the introduction to and use of the stellar evolutionary codes as well as simple analysis of time series data relevant for asteroseismology. The final exam is a written assignment (project report) where the individual students will write a project report in a subject selected from a catalogue with theoretical as well as observational projects." . . "Presential"@en . "FALSE" . . "Projects in stellar evolution"@en . . "5" . "Description of qualifications\nThe aim of the course is to allow in-depth projects and specialisation with a topic linked directly to the lecture course on Advanced Stellar Evolution. The projects are non-obligatory for students that follow the Advanced Stellar Evolution course, but the aim is to coordinate the teaching and content of the Advanced Stellar Evolution course with the projects. The main part of the course will take place in the last 2/3 of the semester in order to allow the student to obtain the needed background following the Advanced Stellar Evolution course. It is required to follow the Advanced Stellar Evolution lecture course in order to follow the project course on Stellar Evolution.\n\n \n\nWhen the course is finished the student is expected to be able to:\n\nPlan and execute a project with a theoretical or practical focus.\nAnalyse data or perform modelling or simulations.\nSearch for relevant scientific literature.\nEvaluate the results and boundary conditions for a specific research project\nCollaborate in smaller groups with the aim of producing a scientific result\nPresent the results as a small talk at a final workshop day.\nContents\nThe course is closely linked to the lecture course on Advanced Stellar Evolution and will focus on in-depth study and specialisation within research on Stellar Evolution. Both theoretical and practical projects are offered. Examples: Modelling, simulations, data analysis, littérature studies. The specific possible projects will be introduced at the start of the course. The project is performed in small groups and under supervision, with support from other staff (incl. postdocs, phd-students, guests, etc.)." . . "Presential"@en . "FALSE" . . "stellar physics"@en . . "5" . "The topics covered by the course: - fundamentals of stellar spectroscopy, observations and analysis - the physical laws and equations of stellar structure, problems related with numerical solutions, examples of computer codes, examples of results - formation of stars, main evolutionary stages, different stellar remnants - nucleosynthesis in stars, mass-loss from stars, explosions, chemical evolution of the Universe - stars exchanging mass in binary systems - variable stars, causes of variability, importance for astrophysics - details of the structure of our Sun - contemporary problems of stellar studies, main unsolved issues" . . "Presential"@en . "TRUE" . . "Advanced topics of stellar structure and evolution"@en . . "5" . "Deepening the knowledge of evolutionary states of various types of stars through expanding \nthe knowledge of physical laws necessary for modeling them. Discussion of issues related to \nthermodynamics, equation of state, energy transport, angular momentum transport and the \neffects of mixing elements in conditions of stellar interiors, cosmic and stellar \nnucleosynthesis. Familiarization with the equations of structure and evolution of stars, \nequations of state for fermions and bosons (in conditions of none, total and partial \ndegeneracy). Getting to know the numerical methods for constructing evolutionary models \nof various types of stars. Getting to know the types of nuclear reactions, cross sections, \nreaction rates, radiation induced reactions, photodisintegration, reactions involving charged \nparticles and reactions involving neutrons. Discussion of changes of the chemical element \nabundances resulting from nuclear processes. Discussion of nuclear reaction cycles (pp, CNO, \nCNO hot cycle, 3alpha, explosive burning helium and other advanced nuclear reaction cycles \ninvolving the burning of carbon, neon, oxygen, silicon)." . . "Presential"@en . "FALSE" . . "Variable stars"@en . . "3" . "Criteria used to classify variable stars. History of the discovery of variable stars, catalogues\nof variable stars. General classification of variable stars, stars exhibiting simultaneously\ndifferent types of variability. Types of Cepheids, use of Cepheids as standard candles, Baade-\nWesselink method, Hertzsprung progression. Pulsating stars in the classical instability strip.\nPulsating stars of the main sequence, Beta Cephei and SPB-type variables. Compact pulsating\nstars (white dwarfs, hot sub-dwarfs). Pulsating types of red giants. The Sun as a pulsating\nstar, solar-type oscillations, their nature and detection methods. Binary stars: classification\ncriteria, proximity effects and tidal effects. Determination of the parameters of the\ncomponents of binary systems (including masses, radii and ages). Cataclysmic and pre-\ncataclysmic stars, novae. Stars exhibiting rotational variability, pulsars. Eclipsing phenomena\nin star-other object (e.g. star-planet) systems. Microlensing, detection methods and use.\nMassive photometric sky surveys – motivations and examples. Variability detection methods,\nautomatic classification of variable stars." . . "Presential"@en . "TRUE" . . "Advanced topics of stellar atmospheres"@en . . "5" . "Introductory information: objectives of stellar atmosphere research, spectral classification. \nModelling of stellar atmospheres: assumptions and equations. Energy transfer mechanisms \n(radiation, convection, diffusion). Interaction of radiation and matter. Atomic data required \nto build a model of the atmosphere. Basic models of atmospheres, assumptions: 1D \ngeometry, assumption of local thermodynamic equilibrium, mixing length theory, blanketing. \nRealistic atmosphere models: 3D geometry, no local thermodynamic equilibrium, stellar wind \nand more. Models of the Sun's atmosphere. Methods of analysis of stellar spectra. \nDetermination of atmospheric parameters (e.g. effective temperature, surface gravity, \nchemical composition)." . . "Presential"@en . "FALSE" . . "Compact stars"@en . . "3" . "Observations of Compact Stars (CS). CS properties. Equation of state for the CS crust Dense\nnuclear matter and quark matter in the CS interior. General relativistic CS structure. Neutrino\nprocesses and CS cooling. CS at birth: Supernovae and protoneutron stars. Gravitational\nwave signals and black hole formation. Exploring CS matter in heavy-ion collision\nlaboratories." . . "Presential"@en . "FALSE" . . "Dynamics of stellar systems 1-2"@en . . "4" . "A comprehensive descripion of the dynamical structure and evoluion of galaxies and other stellar systems\r\n\r\nSemester 1: Introducion; Potenial Theory; Orbits of stars; Equilibria of Collisionless Systems\r\n\r\nSemester 2: Stability of Collisionless Systems; Disk dynamics and spiral structure; Kineic theory; Collisions and encounters; Galaxy formaion" . . "Presential"@en . "FALSE" . . "Evolution of stars and stellar systems"@en . . "6" . "Observations of stars with similar spectral characteristics are linkted to theoretical evolutionary phases of single stars and of binaries. We investigate how to calculte theoretical fractions of stars with similar characteristics and we discuss the influence of physical parameters that critically affect the theoretical predictions. The predictions are then compared to the most recent observations. Finally, we discuss how the various types of stars and stellar populations affect the evolution of galaxies (chemical evolution) and we distinguish elliptical galaxies (single starburst galaxies) and spiral galaxies where starformation proceeds continuously in time.\nALGEMENE COMPETENTIES\r\nTo acquire sufficient knowledge in order to start a masterthesis or a PhD within the research group of the Theoretical Astrophysics of the Vrije Universiteit Brussel. Indeed, the main research subject of the group is the study of large groups of stars, how they evolve, how they contribute to the overal evolution of galaxies." . . "Presential"@en . "FALSE" . . "Stellar evolution"@en . . "8" . "The aim of this course is to give a specialistic overview of the stellar evolution theory for stars with different masses. In particular the student will understand how the main physical properties of stars with different masses change as a function of the age, how these changes are related to the thermonuclear evolution of each star, which are the final stages of star life, which are the properties of the remnants. The student will also get a general view of the open issues in the field of the stellar evolution research." . . "no data"@en . "TRUE" . . "Advanced stellar physics and asteroseismology"@en . . "6" . "This course presents students with the theoretical underpinnings of asteroseismology, i.e. the study of stellar properties based on observations of stellar oscillations. By the end of the module students will be able to explain the nature of normal oscillation modes, and relate them to the characteristics of the internal structure of stars. Students will also appreciate the wider implications of asteroseismology on high-precision stellar physics, on studies of stellar populations, and on the characterisation of exoplanetary systems." . . "no data"@en . "FALSE" . . "Stellar structure and evolution"@en . . "6" . "not available" . . "Presential"@en . "FALSE" . . "Start of semester project"@en . . "no data" . "no data" . . "Presential"@en . "TRUE" . . "Stellar structure and evolution"@en . . "6" . "Specific Competition\nCE1 - Understand the basic conceptual schemes of Astrophysics\nCE2 - Understand the structure and evolution of stars\nCE3 - Understand the mechanisms of nucleosynthesis\nGeneral Competencies\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\n\nTheoretical and practical contents of the subject\nTopics (headings):\n\n1. Stellar observables\n2. Stellar structure equations\n3. Gas equation of state\n4. Thermonuclear power generation\n5. Simple stellar models\n6. The stability of stars\n7. Stellar interior conditions and relationships of homology\n8. Stellar evolution: early evolutionary states\n9. Stellar evolution: late evolutionary states\n10. The end of massive stars: supernovae, pulsars and black holes\n11. Binary stars" . . "Presential"@en . "FALSE" . . "Stellar atmospheres"@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\nCE9 - Understand the instrumentation used to observe the Universe in the different frequency ranges\nGeneral Competencies\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\n\nTheoretical and practical contents of the subject\n- Lecturer: ARTEMIO HERRERO\n- Topics (headings):\n1.- Spectral Types. Stellar atmospheres in Astrophysics.\n2.- The radiative transport equation. Absorption and emission coefficients. Optical depth. Source function\n3.- Atomic populations. ETL and NETL. Statistical Equilibrium Equations.\n4.- Atmosphere models in hydrostatic equilibrium\n5.- Deviations from hydrostatic equilibrium: Stellar winds\n6.- Spectral analysis" . . "Presential"@en . "FALSE" . . "Stellar astronomy"@en . . "5,0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "Stellar photometry"@en . . "6,0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "Stellar atmospheres and interstellar medium"@en . . "6,0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "Variable stars"@en . . "5,0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "Pulsating stars"@en . . "4.0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "Stars and galaxies"@en . . "20.0" . "#### Prerequisites\n\n* Foundations of Physics 1 (PHYS1122) AND ((Single Mathematics A (MATH1561) and Single Mathematics B (MATH1571)) OR (Calculus I (MATH1061) and Linear Algebra I (MATH1071))).\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 provides an introduction to Astronomy and the foundations for Astrophysics courses in later years.\n\n#### Content\n\n* The syllabus contains:\n* Telescopes; Binary stars and Stellar Parameters; The Classification of Stellar Spectra; Stellar Atmospheres; The Interior of Stars; The Sun; The Process of Star Formation; Post-Main-Sequence Stellar Evolution; Stellar Pulsation; The Degenerate Remnants of Stars; Black Holes; Close Binary Systems; The Milky Way Galaxy; The Nature of Galaxies; Galactic Evolution.\n\n#### Learning Outcomes\n\nSubject-specific Knowledge:\n\n* Having studied this module students will be aware of the basic techniques of observational astronomy.\n* They will understand the basic physics of stellar interiors.\n* They will appreciate why we see stars of widely differing colours and brightnesses.\n* They will have had their understanding of stellar properties and physics extended to pulsating and binary stars.\n* They will have an introductory knowledge of galactic and extragalactic astronomy.\n\nSubject-specific Skills:\n\n* In addition to the acquisition of subject knowledge, students will be able to apply the principles of physics to the solution of predictable and unpredictable 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 tutorial-style workshops.\n* The lectures provide the means to give a concise, focused presentation of the subject matter of the module. The lecture material will be defined by, and explicitly linked to, the contents of recommended textbooks for the module, thus making clear where students can begin private study. When appropriate, the lectures will also be supported by the distribution of the 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 other mutually convenient times.\n* Student performance will be summatively assessed through an open-book examination and formatively assessed through problem exercises and a progress test. The open-book examination will provide the means for students to demonstrate the acquisition of subject knowledge and the development of their problem-solving skills. The problem exercises, progress test and workshops will 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/PHYS2621" . . "Presential"@en . "TRUE" . . "Stellar structure and evolution"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua_\n\n### Objectives\n\nThe main objective is to learn the fundamental principles that establish the internal structure and evolution of stars. To do so it is required to study in detail what are stars, their most important features and how stars work. A detailed formulation of the problem is covered by defining the equations of stellar structure and the physical relations, together with a careful identification of the relevant boundary conditions that determine the solution that represents the observations. Thus the student learns how to apply the physical principles to interpret the different phases of a star’s life, using the observations to validate the model. Some topics of active research are addressed in order to consolidate the concepts and techniques being discussed, allowing the student to learn with applications to specific/real cases.\n\n### Learning outcomes and competences\n\nIn order to acquire a solid understanding of the fundamental principles of stellar physics and how stellar models can be validated with the observations, the program is defined including the physics and mathematical principles required by stellar structure and evolution models. The program includes the concepts required to construct the model and the discussion on how this model can predict the expected observational behavior of stars, supporting the confrontation between models and astronomical observations in regimes not available in the laboratory. Thus, the contents include not only the theoretical formulation of the relevant fundamental concepts but also the detailed discussion of the observational information that is avaliable and how it can be interpreted using the models from the theoretical analysis.\n\n### Working method\n\nPresencial\n\n### Program\n\n \n2. Observation of stars and clusters\n \n4. Stellar structure equations\n \n6. Physical relations relevant for the stellar interior\n \n8. Description of the internal structure of a star and its evolution\n \n10. Methods for study of solar/stellar interior\n \n12. Ongoing research topics and open questions\n \n\n### Mandatory literature\n\nR. Kippenhahn; [Stellar structure and evolution](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000226469 \"Stellar structure and evolution (Opens in a new window)\"). ISBN: 3540502114 \n\n### Complementary Bibliography\n\nClayton Donald D.; [Principles of stellar evolution and nucleosynthesis](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000224824 \"Principles of stellar evolution and nucleosynthesis (Opens in a new window)\"). ISBN: 0-226-10953-4 (pbk) \nC. J. Hansen; [Stellar interiors](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000227823 \"Stellar interiors (Opens in a new window)\"). ISBN: 0-387-94138-X \n\n### Comments from the literature\n\nReferences (books and reserach articles) on specific sections of the program are provided in the lecture notes and/or during the lectures.\n\n### Teaching methods and learning activities\n\nThe contents are discussed in the class by using the blackboard and the projection of plots. In the final part there is the discussion of scientific articles. Along the semester some time is used to solve exercises/examples, made available in the lecture notes. All course material is available through the Aulas na Web, including a copy of the slides used, the exercises, and the lecture notes for stellar structure and evolution. There is a reference book that is used as the primary reference, but for some itens complementary books and/or scientific articles are also provided.\n\n \n\n \n\nTeaching is organized to enable the acquisition of the formalism that describe how stars work (Chapters 2, 3 and 5), while other components develop the capacity to analyze the observations and interpret them based on the formalism being discussed (chapters 1 and 4). To do so, the lectures are a combination of theoretical discussion of the physics, identification of typical applications of stellar astronomy, and problem solving, always with emphasis on the participation of the student. Chapter 6 seeks to use active research topics to reinforce the importance of the concepts discussed and to allow the student to recongnize the value of what is learned in the various chapters, as a necessary and useful tool for research in stellar physics.\n\n### keywords\n\nPhysical sciences \nPhysical sciences > Astronomy \nPhysical sciences > Astronomy > Astrophysics \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nPresentation/discussion of a scientific work: 25,00%\nExam: 70,00%\nPresential participation: 5,00%\n\n**Total:**: 100,00%\n\n### Amount of time allocated to each course unit\n\nPresentation/discussion of a scientific work: 30,00 hours\nAutonomous study: 90,00 hours\nFrequency in classes: 42,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nThe student will not be able to complete the course if he/she does not participate in half of the lectures. There will be an attendance log in all classes.\n\n### Calculation formula of final grade\n\nThe final rating has the following components:\n\n1. 14 points - the final written exam with consultation (minimum grade is required in this component of one third)\n2. 5 points - presentation and discussion of a topic\n3. 1 point - active participation in classes, to be evaluated by submitting questions, solutions for problems to be proposed, discussion of the individual work and its progress, discussion of research articles, etc.\n\nThe student may request an additional assessment as allowed by the Evaluation Regulation of FCUP.\n\n### Examinations or Special Assignments\n\nThe presentation will be a review of a current research topic: it aims to ask students to produce a detailed review of topic on Stellar Structure and Evolution. The choice of topic is made at the beginning of the semester, and students are expected to look for additional/complementary information, namely in scientific articles (for example in the Astrophysics Data System or in specific journals). \n \nThe presentation and its discussion will take place at the end of the semester. The evaluation is associated with: \n \n\n \n* depth of the topic addressed; scope of the topics discussed; clarity in approach and proper description\n \n* well-structured and clear presentation, with relevant and easy-to-read slides, including useful figures and correctly planned for the time available.\n \n* capacity to have a in deep discussion, which demonstrates having understood the topics presented, showing copacity to argue and clarify the content that was presented.\n \n\n \n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498805" . . "Presential"@en . "TRUE" . . "Stellar formation and circum-estelar medium"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua._\n\n### Objectives\n\nThe processes associated with the formation and the early evolution of stars are introduced. The period in analysis includes the molecular clouds formation, the formation of the proto-star and the pre-main-sequence evolution before the star reaches the main sequence. Complementing the theoretical part, we present observational examples of the different stages of evolution of a young star.\n\n### Learning outcomes and competences\n\nAt the end the student will have a global view of the theories of star formation and pre-main sequence stellar evolution. The student will also have a global view over the observational component that is used for the study of molecular clouds, protostars and circumstellar medium.\n\n### Working method\n\nPresencial\n\n### Program\n\nI - Star Formation in our Galaxy\n\n1\\. Overview\n\n1. Stellar Nurseries\n2. Stars and their evolution\n3. The Galactic context\n\n2\\. Interstellar Medium (ISM)\n\n1. Galactic Gas\n2. Phases of the ISM\n3. Insterstellar Dust - Extinsion/Emission - Properties of the grains\n\n3\\. Molecular Clouds\n\n1. Giant Molecular Clouds\n2. Virial Theorem Analysis\n3. Dense Cores\n\n4\\. Young Stellar Systems\n\n1. Embebed Clusters\n2. The Initial Mass Function\n\nII - Physical Processes in Molecular Clouds\n\n1\\. Introduction to Radiative Transfer \n \n2\\. Molecular Transitions\n\n1. Interstellar Molecules\n2. Hydrogen (H2)\n3. Carbon-Monoxide (CO)\n4. Applications of CO\n\n3\\. Heating and Cooling\n\n1. Cosmic Rays\n2. Interstellar Radiation\n3. Cooling by Atoms, Molecules and Dust\n\n4\\. Cloud Thermal Structure\n\n1. The Buildup of Molecules\n2. The Molecular Interior\n\nIII - From Clouds to Stars\n\n1\\. Cloud Equilibrium and Stability\n\n1. Isothermal Spheres and the Jeans Mass\n2. Magnetostatic Configurations\n\n2\\. The Collapse of Dense Cores\n\n1. Ambipolar Diffusion\n2. Inside-Out Collapse\n\n3\\. Protostars\n\n1. First Core and Main Accretion Phase\n\n4\\. Multiple Star Formation\n\n1. Dynamical Fragmentation of Massive Clouds\n\nIV - Pre-Main Sequence Stars\n\n1 - T-Tauri Stars\n\n1. Line and Continuum Emission\n2. Outflow and Infall\n3. Circunstellar Disks\n4. Post-T Tauri Stas and Beyond\n\n2 - Herbig Ae/Be Stars\n\n1. Basic Properties\n2. Gaseous and Debris Disks\n\nV - Accretion discs \n1\\. Theory of standard accretion discs \n\n1. Equations of conservation and the difusion equation\n2. Stationary discs\n3. Boundary conditions\n\n2\\. Observations vs Theory \n\n1. Spectral Energy distribution\n2. Spectral emission from an optically thick steady disc\n3. Sources of excess emission\n\n3\\. Introduction to accretion shock models\n\n### Mandatory literature\n\nStahler Steven W.; [The formation of stars](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000263483 \"The formation of stars (Opens in a new window)\"). ISBN: 3-527-40559-3 \nFrank J.; [Accretion power in astrophysics](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000244780 \"Accretion power in astrophysics (Opens in a new window)\") \n\n### Complementary Bibliography\n\nLee Hartmann; Accretion Processes in Star Formation, Cambridge University Press, 2009. ISBN: 978-0-521-53199-3 \nDonald E. Osterbrock; [Astrophysics of gaseous nebulae and active galactic nuclei](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000226259 \"Astrophysics of gaseous nebulae and active galactic nuclei (Opens in a new window)\"). ISBN: 0-935702-22-9 \nGray David F.; [The observation and analysis of stellar photospheres](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000268080 \"The observation and analysis of stellar photospheres (Opens in a new window)\"). ISBN: 0-521-85186-6 \nPhilip J. Armitage; Astrophysics of Planet Formation, Cambridge University Press, 2010. ISBN: 978-0-521-88745-8 \n\n### Teaching methods and learning activities\n\nMultimedia presentations and Tutorial guidance. \n \nThe support material of the course will be available via the Moodle UP, including a copy of the slides used. There is a main reference book that is the main bibliography, but for some components of the course complementary bibliography and/or scientific articles may be used.\n\n### Software\n\nPython \nLatex \n\n### keywords\n\nPhysical sciences \nPhysical sciences > Astronomy \nPhysical sciences > Astronomy > Astrophysics \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nExam: 70,00%\nPractical assignment or project: 30,00%\n\n**Total:**: 100,00%\n\n### Amount of time allocated to each course unit\n\nPresentation/discussion of a scientific work:10,00 hours\nAutonomous study: 70,00 hours\nFrequency of lectures: 42,00 hours\nWritten assignment: 40,00 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 1/3 of the planned classes.\n\n### Calculation formula of final grade\n\nThe final grade is obtained through three components: \n1) 70% - a final written exam \n2) 20% - computational work developped during the semester with a final written report \n3) 10% - presentation and discussion of the computational work.\n\n### Examinations or Special Assignments\n\nPratical work task with written report and presentation. This task will be done throughout the semester.\n\n### Classification improvement\n\nThe student may improve the classification in the written exam (weight of 70% in the final classification). It will not be possible to improve the classification in the pratical work task\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498808" . . "Presential"@en . "TRUE" . . "Star formation and structure"@en . . "6.0" . "Competences to be gained during study\n\n— Capacity to write scientific and technical documents.\n\n— Capacity to communicate, give presentations and write scientific articles on fields related to the topics covered in the master’s degree.\n\n— Capacity to test predictions from theoretical models with experimental and observational data.\n\n— Capacity to critically analyze the results of calculations, experiments or observations, and to calculate possible errors.\n\n \n\n--Capacity to elaborate scientific proposals concerning to a topic of the course program.\n\n-Capacity to analyze observational data from radiointerferometers using CASA tool.\n \n\nLearning objectives\n\nReferring to knowledge\n\n— Learn basic concepts on the physics of the interstellar medium, with a focus on processes relating to star formation in our galaxy and the pre-main-sequence star evolution of objects in different mass ranges (low, intermediate and high).\n\n \n\n— Deepen knowledge of the application of basic physics to gravity, hydrostatic equilibrium, heat transport and nuclear reactions to understand the structure and evolution of stars and gain a vision of current problems of interest in star formation and young stellar object evolution.\n\n \n\n \n\nTeaching blocks\n\n \n\n1. Introduction\n1.1. The Milky Way galaxy\n\n1.2. The interstellar medium\n\n2. The tools: radio interferometry. Optical and near-infrared astronomy\n3. Interstellar medium and star-forming regions\n3.1. Interstellar dust; Composition and physical properties; Extinction, reddening and polarisation; Thermal emission\n\n3.2. Atomic, ionised and molecular gas; Spectral line emission; Free-free emission, recombination lines of HII and physical parameters from HII; Chemistry of the molecular gas and formation of molecules; Molecular lines and physical parameters of molecular-line observations\n\n3.3. Astrochemistry\n\n3.4. Energy balance in molecular clouds; Virial theorem; Turbulence and magnetic field; Magnetically supported cores\n\n3.5. Molecular clouds; Morphology, filaments and dense cores; Sites of star formation, examples of TMC, Orion\n\n4. Young stellar objects\n4.1. Spectral energy distribution; Classification and observational properties of YSO\n\n4.2. PMS evolution; Hayashi and Henyey tracks; ZAMS\n\n4.3. T Tauri stars and Ae/Be stars; Models and observations\n\n4.4. Interaction of YSO with their environment; Jets, Herbig-Haro objects and bipolar molecular outflows\n\n4.5. Accretion and supersonic ejection processes in YSO; Accretion disks; Observation and models\n\n5. Practical cases\n5.1. Basic concepts on calibration and imaging with CASA\n\n5.2. Proposal writing\n\n \n\n \n\nTeaching methods and general organization\n\n \n\n— Lectures.\n\n— Seminars led by guest experts.\n\n— Discussion of recently published articles.\n\n— Discussion of projects presented by the students.\n\n—Discussion of a practical case elaborated from file data, applying observational techniques studied in the course.\n\n--Elaboration of observational proposals \n\n \n\n \n\nOfficial assessment of learning outcomes\n\n \n\nContinuous assessment consists of:\n\n— Submission of short written exercises or problems on the course content to be solved at home.\n\n— An assignment on a topic related to the course contents. This includes a written report (limited length) and an oral presentation (15 minutes).\n\n—A practical case elaborated from file data, applying observational techniques studied in the course\n\nThis part is worth 40% of the final grade.\n\n— Final written examination, consisting of short-answer questions on physical concepts explained throughout the course.\n\nThe final exam is worth 60% of the final grade.\n\nRepeat assessment consists of a written examination, similar to that in continuous assessment, worth 100% of the final grade.\n\n \n\nExamination-based assessment\n\nSingle assessment consists of the oral presentation of an assignment, similar to that in the continuous assessment, and a written examination with questions on the course content and problem-solving exercises.\n\n \n\n \n\nReading and study resources\n\nCheck availability in Cercabib\n\nBook\n\nPrialnik, Dina. An Introduction to the theory of stellar structure and evolution. 2nd ed. Cambridge : Cambridge University Press, 2010 Enllaç\n\nhttps://cercabib.ub.edu/discovery/search?vid=34CSUC_UB:VU1&search_scope=MyInst_and_CI&query=any,contains,b1494539* Enllaç\n\nEstalella, Robert ; Anglada Pons, Guillem. Introducción a la física del medio interestelar. Barcelona : Publicacions i Edicions de la Universitat de Barcelona, 2008 (Textos docents ; 50) Enllaç\n\n \tThis book covers most of the contents of the course.\n\n2a ed. Enllaç\nhttps://cercabib.ub.edu/discovery/search?vid=34CSUC_UB:VU1&search_scope=MyInst_and_CI&query=any,contains,b1312542* Enllaç\nhttps://cercabib.ub.edu/discovery/search?vid=34CSUC_UB:VU1&search_scope=MyInst_and_CI&query=any,contains,b1278664* Enllaç\n\nHartmann, Lee. Accretion processes in star formation. 2nd ed. Cambridge : Cambridge University Press, 2009 Enllaç\n\n\nSmith, Michael D. The origin of stars. London : Imperial College Press, cop. 2004 Enllaç\n\n\nStahler, Steven William ; Palla, F. The formation of stars. Weinheim : Wiley-VCH, 2004 Enllaç\n\n\nWard-Thompson, Derek ; Withworth, Antony P. An introduction to star formation. Cambridge : Cambridge University Press, 2011 Enllaç\n\n\n\"Interstellar and Intergalactic Medium Barbara Ryden & Richard W. Pogge Cambridge University Press, 2021 \n\nMore information at: http://grad.ub.edu/grad3/plae/AccesInformePDInfes?curs=2023&assig=568425&ens=M0D0B&recurs=pladocent&n2=1&idioma=ENG" . . "Presential"@en . "FALSE" . . "Biological and environmental sciences honours project start"@en . . "40.0" . "Module Description\nThe Honours dissertation project runs through your entire final year and allows you to carry out an original piece of scientific research on a subject of your choice covering contemporary biological and environmental sciences.\n\nThis is your opportunity to do some independent in-depth analysis on a topic that most excited you during your undergrad studies. During the project you'll have the guidance and advice of a dedicated supervisor. This module covers the start of your honours project and ensures that you have submitted your project for ethical approval, you have reviewed the relevant literature, and you have a project plan to put you on the pass to successfully complete your final dissertation in the spring semester.\n\nThese steps will be supported by a series of seminars. The data collection for your dissertation can start at any point once you have received ethical approval for your project and is not limited to the spring semester.\n\nLocation/Method of Study\nStirling/On Campus, UK\n\nModule Objectives\nProject specific work aimed at formulating the research question and/or hypothesis.\n\nPreparation of the first chapter of the thesis\n\nA series of prescribed sessions on the ethics application procedure.\n\nProject specific training and optional participation in the BES research seminar and PhD seminar series.\n\nAdditional Costs\n£TBC If the project requires fieldwork, there could be additional costs associated with travel to the field site. This is project specific, therefore please discuss with your potential supervisor.\n\nCore Learning Outcomes\nOn successful completion of the module, you should be able to:\n\nassess the ethical implications of your project and submit an ethics application for approval;\ncritically analyse scientific evidence and arguments from the peer-reviewed literature relevant to your research project;\nidentify a knowledge gap and construct a feasible and succinct research proposal.\nIntroductory Reading and Preparatory Work\nPlease contact your supervisor for a list of readings that is appropriate to your project.\n\nA more general text we recommend is the following (available from the library):\n\nFisher, Elizabeth; Thompson, Richard: Enjoy Writing Your Science Thesis or Dissertation!  - a Step-by-Step Guide to Planning and Writing a Thesis or Dissertation for Undergraduate and Graduate Science Students. Second edition, London, Imperial College Press, 2014.\n\nDelivery\nDirected Study\t22 hours\tA discussion or classroom session focussing on particular topics or projects, may be virtual but are available at a specific time or live\nDirected Study\t8 hours\tA meeting involving one-to-one or small group supervision, feedback or detailed discussion on a particular topic or project, online or in person\nUndirected Study\t170 hours\tIndependent activities required to complete the module\nTotal Study Time\t200 hours\t\nAttendance Requirements\nThe seminars consist\n(a) of a series of prescribed sessions on the ethics application procedure, literature review etc.\n(b) optional participation in the BES research seminar and PhD seminar series.\n\nAssessment\n% of final\ngrade\tLearning\nOutcomes\nCoursework\t0\t1\nCoursework\t60\t2\nResearch Proposal\t40\t2,3\nCoursework: 100%\n\nMore information at: https://portal.stir.ac.uk/calendar/calendar.jsp?modCode=SCIU9PS&_gl=1*12l877f*_ga*MTY1OTcwNzEyMS4xNjkyMDM2NjY3*_ga_ENJQ0W7S1M*MTY5MjAzNjY2Ny4xLjEuMTY5MjAzODQ1My4wLjAuMA.." . . "Presential"@en . "TRUE" . . "Star formation and interstellar medium"@en . . "8" . "no data" . . "Presential"@en . "TRUE" . . "Stellar structure and stellar evolution"@en . . "8" . "no data" . . "Presential"@en . "TRUE" .