. "Physics"@en . . "Astronomy"@en . . "English"@en . . "Mathematics"@en . . "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" . . "General relativity"@en . . "6.0" . "### Teaching language\n\nSuitable for English-speaking students\n\n### Objectives\n\nThe aim is to introduce the main ideas about the general theory of relativity, according to which the space-time curvature and dynamics are determined by its energy-matter content. For reach this level of understanding, the physical and mathematical principles of this formulation will be discussed. \n \nTo develop skils in theoretical physics.\n\n### Learning outcomes and competences\n\nAdquire the geometrical concepts associated to Einstein gravity, as well as the importance of this theory to describe physical phenomena.\n\n### Working method\n\nÀ distância\n\n### Program\n\n1\\. Special Relativity - Lorentz group and transformations - Vectors e Tensors - Electrodynamics 2. Einstein's Equivalence Principle - Clock Postulate and the Universality of the gravitational redshift and the geodesic deviation - Weak Equivalence Principle - Covariance under local Lorentz transformations - Covariance under position transformations - Schiff's conjecture - Princípio de Equivalência Forte 3. Generalized Covariance Principle 4. Introduction to Differential Geometry - Manifolds - Exterior derivative and Lie derivative - Covariant derivative - Curvature tensor - Metric 5. Einstein's General Relativity - Energy-Momentum tensor - Einstein's field equations - Newtonian limit, linear approximation of Einstein's field equations and gravitational waves - Matter fields - Lagrange formulation (Einstein-Hilbert action, bosonic string action and corrections to the Einstein-Hilbert action) - Classic tests: Deflection of light and radar eco delay in the vicinity of the sun, and advance precession of Mercury's perihelion 6. Exact Solutions of Einstein's field equations - Minkowski, De Sitter e anti-De Sitter space-time - Schwarzschild's black hole solution - Robertson-Walker space-time Bibliography: - S. Weinberg, \\`\\`Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity'' (John Wiley and Sons, New York 1972). Chapters: 1, 2, 3, 4, 7, 8. - S.W. Hawking and G.F.R. Ellis, \\`\\`The Large Scale Structure of Space-Time'' (Cambridge University Press, Cambridge 1973). Chapters: 1, 2, 3. - C.W. Misner, K.S. Thorne and J.A. Wheeler, \\`\\`Gravitation'' (Freeman, San Francisco, 1974). - \\`\\`300 Years of Gravitation'', Eds. S.W. Hawking and W. Israel (Cambridge University Press, Cambridge 1987). Capítulos: 4 e 5. - R.M. Wald, \\`\\`General Relativity'', (The University of Chicago Press, Chicago 1984). Chapters: 1, 2, 3, 4, 5, 6. - C.M. Will, \\`\\`Theory and experiment in gravitational physics'' (Cambridge University Press, Cambridge 1993). Capítulos: 1, 2, 3 e 14. - G.G. Ross, \\`\\`Grand Unified Theories'' (Benjamin/Cummings, Menlo Park, California 1984). Chapters: 2, 3, 4 and 12. - M.B. Green, J.H. Schwarz and E. Witten, \\`\\`Superstring Theory Vol. 1 Introduction'' (Cambridge University Press, 1987). Chapters: 2. - E.W. Kolb e M.S. Turner, \\`\\`The Early Universe'' (Addison-Wesley P. C., 1990). Chapters: 1, 3, 4, 5 and 8. - P.J.E. Peebles, D.N. Schramm, E.L. Turner e R.G. Kron, Nature, 352 (1991) 769. - O. Bertolami, \\`\\`Modelo Cosmológico Padrão: uma breve introdução'', \"Agregação\" lecture, Instituto Superior Técnico, July 1996.\n\n### Mandatory literature\n\nSchutz Bernard F.; [A first course in general relativity](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000224998 \"A first course in general relativity (Opens in a new window)\"). ISBN: 0-521-25770-0 \n\n### Complementary Bibliography\n\nHawking Stephen 1942-2018; [The large scale structure of space-time](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000233043 \"The large scale structure of space-time (Opens in a new window)\"). ISBN: 0521200164 \nS. Weinberg; Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity \nWeinberg Steven; [Gravitation and cosmology](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000238852 \"Gravitation and cosmology (Opens in a new window)\"). ISBN: 0-471-92567-5 \n\n### Teaching methods and learning activities\n\nTheory and problem solving lectures.\n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nExam: 75,00%\nWritten assignment: 25,00%\n\n**Total:**: 100,00%\n\n### Amount of time allocated to each course unit\n\nDevelopment of report/dissertation/thesis: 30,00 hours\nAutonomous study: 90,00 hours\nFrequency of lectures: 42,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nAttendance of theoretical/pratical lectures.\n\n### Calculation formula of final grade\n\nThe final mark has a 75% component from the exam and a component of 25% from a written essay also presented orally. The minimum grading for the exam is 8.\n\n### Classification improvement\n\nSecond examination round for the exam mark (75% of the total mark).\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509988" . . "Presential"@en . "TRUE" . . "Spectroscopy and photometry in astronomy"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua._\n\n### Objectives\n\nIt is intended that students understand the workings and characteristics of detectors and instruments of observation in modern astronomy, in particular in the optical waveband and including CCD cameras and spectrographs. They should also acquire the basic knowledge enabling them to reduce photometric and spectroscopic data, analyze the results and infer conclusions on practical applications in research.\n\n### Learning outcomes and competences\n\nFamiliarization with the basic signals in Astronomy (photometry, spectroscopy), detectors and their operation in order to be able to reduce the respective data. Acquisition of basic knowledge on data reduction. Ability to handle specific software and analyse the results of its application to real data.\n\n### Working method\n\nPresencial\n\n### Program\n\n1\\. Instrumentation in Astronomy - Cameras and detectors. - Noise and artifacts recorded on a CCD and their correction. - Filter and magnitude systems in the optical. - The spectrograph and the dipersor - gratings. - Resolving power of a spectrograph. - Quick reference to multi-object spectroscopy and integral field spectroscopy. 2. Reduction of low-resolution spectroscopic observations - The treatment of thermal noise and sensitivity analysis of the detector. - Removal of the effects of cosmic rays in the images. - Calibration of the spectra in wavelength. - Calibration of spectra in flux using standard reference stars. - Analysis 3. Reduction of observations in several photometric filters - The treatment of thermal noise and sensitivity analysis of the detector. - PSF analysis and detection of objects in the image. - Aperture photometry. - Photometry calibration using standard stars.\n\n### Mandatory literature\n\nSterken Chr.; [Astronomical photometry](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000228193 \"Astronomical photometry (Opens in a new window)\"). ISBN: 0-7923-1776-9 \nKitchin C. R.; [Astrophysical techniques](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000193071 \"Astrophysical techniques (Opens in a new window)\"). ISBN: 0-85274-461-7 \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 \n\n### Complementary Bibliography\n\nSutton Edmund C.; [Observational astronomy](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000295338 \"Observational astronomy (Opens in a new window)\"). ISBN: 9781107010468 \n\n### Comments from the literature\n\nSupport documents regarding the software used for data reduction will be made available or indicated to the students. Published scientific papers will also be given as bibliographic material, when/if required.\n\n### Teaching methods and learning activities\n\nPractical work with computer during classes, enabling the reduction of real astronomical data using the adopted software. These classes will be supplemented with lectures on the fundamentals of data processing. The final exam will use the computer, in order to reduce real observations, both spectroscopic and photometric.\n\n### Software\n\nAstropy \n\n### keywords\n\nPhysical sciences > Astronomy \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nTest: 100,00%\n\n### Amount of time allocated to each course unit\n\nEstudo autónomo: 106,00 hours\nFrequency of lectures: 56,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nStudents should participate in, at least, 50% of the practical classes.\n\n### Calculation formula of final grade\n\nStudetns can choose between two alternative assessment systems: \n \nA- With continuous assessment \nA1. \\[50%\\] Intermediate written test on Photometry \nA2. \\[50%\\] Intermediate written test on Spectroscopy \n \nB- Without continuous assessment \nAppeal exam with two components: Photometry \\[50%\\] + Spectroscopy \\[50%\\]\n\n### Classification improvement\n\nBy exam, in the \"época de recurso\" (appeal). The appeal exam will have two components: a module on spectroscopy and another one on photometry. If the student wishes, he/she can improve the grade in only one of the modules.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498802" . . "Presential"@en . "TRUE" . . "Planetary systems"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua._\n\n### Objectives\n\n• Introduce the students to the field of planetary system science, giving them all the tools to understand the concepts and terminology used; \n• Introduce the basic processes of planet formation as an outcome of the stellar formation process; \n• Familiarize the students with the basic theoretical and observational tools used in this domain; \n• Introduce the state-of-the-art research and results; \n• Use the planetary sciences domain to apply concepts of physics and astrophysics that were previously learned.\n\n### Learning outcomes and competences\n\nAt the end of the course, the student should: \n \n• Have a historical perspective about the discovery of our Solar System and of other planetary systems; \n• Describe the characteristics of the Solar System bodies as well as their composition and structure; \n• Have a background about the dynamics of planetary orbits; \n• Recognize the basic steps of the formation of a solar-type star, and how those steps lead to the necessary conditions for planet formation; \n• Have a general view about the process of planetary system formation and evolution, including some details about the formation of our own Solar System; \n• Describe the characteristics of extra-solar planetary systems; \n• List and describe the techniques used in this field of research as well as what astrophysical and physical information they provide; \n• Recognize the limitations and caveats of the different techniques; \n• Describe the difficulties and open issues in this field of research; \n• Describe the present state-of-the-art knowledge about the research in planetary system sciences; \n• Have an overall view about the challenges for the next years in this field, as well as about the major projects that will allow to give the next big steps; \n• Discuss in a critical way all the results in the field; \n• Read and present a scientific paper on planetary system research, and motivate an observational project in the field; \n• Analyze in a qualitative and quantitative way sets of data coming from planet search programs and determine from them the physical parameters of extra-solar planets.\n\n### Working method\n\nPresencial\n\n### Pre-requirements (prior knowledge) and co-requirements (common knowledge)\n\nBasic physics and mathematics.\n\n### Program\n\nTheoretical component: \n \n1\\. The Solar System: a Historical Perspective \n \n2\\. Basic dynamics \n \n3\\. An introduction to the Solar System: general properties and basic concepts \n \n4\\. Star formation: a brief overview \n \n5\\. Disks as planet formation stages \n \n6\\. Planet formation: from observational evidence to basic modelling \n \n7\\. Searching for exoplanets: detection methods \n \n8\\. Stellar Astrophysics and Exoplanets \n \n9\\. The properties of planetary systems \n \n \nPractical components: \n \na. Class excercises \n \nb. Detecting an exoplanet with RV and transit data \n \nc. Presentation of one scientific paper\n\n### Mandatory literature\n\nDe Pater Imke; [Planetary sciences](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000293695 \"Planetary sciences (Opens in a new window)\"). ISBN: 9780521853712 \n\n### Complementary Bibliography\n\nS. Seager; Exoplanets, University of Arizona Press, 2011 \nR.W. Hilditch; An introduction to close binary systems, Cambridge University Press, 2001 \n\n### Teaching methods and learning activities\n\nTheoretical classes. \nPractical component includes the presentation of research papers, the resolution of exercises, and a computational work (and respective report).\n\n### Software\n\nlatex \nhttp://www.astro.up.pt/resources/soap-t \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nExam: 50,00%\nPresential participation: 5,00%\nWritten assignment: 45,00%\n\n**Total:**: 100,00%\n\n### Amount of time allocated to each course unit\n\nAutonomous study: 120,00 hours\nFrequency of lectures: 42,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nFrequency of classes is not mandatory but is considered of great importance, and counts for the final evaluation.\n\n### Calculation formula of final grade\n\nWeighted average of the 3 components: \n\\- Written exam (50%) - minimum 7 (in 20) values \n\\- Exercises about the subjects done during the classes (5%) \n\\- Report of practical work and presentation of scientific paper (45%)\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498804" . . "Presential"@en . "TRUE" . . "Cosmology"@en . . "6.0" . "### Teaching language\n\nEnglish\n\n### Objectives\n\nThe overall objective of this lecture course is to develop in the students an interest in cosmology, communicating to them in a consistent fashion the basic principles as well as the latest developments in this area.\n\n### Learning outcomes and competences\n\nAfter the frequency of this lecture course, students should be able to: understand the fundamental assumptions behind the standard cosmological model; deduce the equations that describe the dynamics of the Universe; describe the observational evidence of the standard cosmological model; understand the successes and limitations of the standard cosmological model; understand the thermodynamic processes most relevant in cosmology, in particular recombination and primordial nucleosynthesis; describe the observational constraints on cosmological parameters and their consequences for the evolution of the Universe; understand the relevance of scalar fields in cosmology, particularly in solving some of the problems of the standard cosmological model; understand the linear and nonlinear evolution of fluctuations in the density of matter in different eras and scales; understand the mechanisms responsible for the anisotropy of the cosmic microwave background and its relation to the large-scale structure of Universe; describe the observational evidence for dark matter and dark energy. This course also aims to develop a wide range of complementary skills in various areas, such as personal and inter-personal organization, written and oral communication, culture in physics and astronomy and the search and selection of bibliography.\n\n### Working method\n\nPresencial\n\n### Program\n\n**1\\. Introduction**\n\n1.1 Basic concepts in Astronomy\n\n1.2 Relevant observations for Cosmology\n\n1.3 Revison of concepts in Special and General Relativity\n\n**2\\. The expanding Universe**\n\n2.1 The cosmological principle\n\n2.2 The Robertson-Walker metric\n\n2.3 The cosmological redshift\n\n2.4 Peculiar velocities\n\n2.5 Equation of state\n\n**3\\. Relativistic cosmology**\n\n3.1 Friedmann equation: deduction and solutions\n\n3.2 Cosmological horizons and the age of the Universe\n\n3.3 Angular and luminosity cosmological distances\n\n**4\\. The primordial Universe**\n\n4.1 Cronology\n\n4.2 Particles in thermal equilibrium\n\n4.3 Entropy\n\n4.4 Decoupling of relativistic and non-relativistic particles\n\n4.5 Primordial nucleosynthesis\n\n4.6 The cosmic microwave background\n\n**5\\. Inflation**\n\n5.1 Problems in the standard cosmological model\n\n5.2 Inflationary models\n\n**6\\. Large-scale structure formation in the Universe**\n\n6.1 Linear evolution of density perturbations\n\n6.2 Transfer functions\n\n6.3 Evolution of non-linear density perturbations\n\n6.4 Statistical description of density and velocity fields\n\n6.5 Observational characterization of large-scale structure: distribution of galaxies, properties of the intergalactic medium, gravitational lensing.\n\n6.6 Temperature and polarization anisotropies in the cosmic microwave background\n\n6.7 Estimation of observational cosmological parameters: general methods, baryon acoustic oscillations and properties of galaxy clusters.\n\n### Mandatory literature\n\nRoos Matts; [Introduction to cosmology](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000263009 \"Introduction to cosmology (Opens in a new window)\"). ISBN: 0-470-84910-X \nLiddle Andrew; [An introduction to modern cosmology](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000263013 \"An introduction to modern cosmology (Opens in a new window)\"). ISBN: 0-470-84835-9 \nRyden Barbara; [Introduction to cosmology](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000291071 \"Introduction to cosmology (Opens in a new window)\"). ISBN: 0-8053-8912-1 \n\n### Complementary Bibliography\n\nWeinberg Steven 1933-; [Cosmology](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000285334 \"Cosmology (Opens in a new window)\"). ISBN: 978-0-19-852682-7 \nDodelson Scott; [Modern cosmology](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000279002 \"Modern cosmology (Opens in a new window)\"). ISBN: 0-12-219141-2 \nPeacock J. A.; [Cosmological physics](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000228133 \"Cosmological physics (Opens in a new window)\"). ISBN: 0-521-42270-1 \nMo Houjun; [Galaxy formation and evolution](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000295217 \"Galaxy formation and evolution (Opens in a new window)\"). ISBN: 9780521857932 \nColes Peter; [Cosmology](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000259888 \"Cosmology (Opens in a new window)\"). ISBN: 0-471-48909-3 \n\n### Teaching methods and learning activities\n\nIn the lecture classes the contents in the program are taught and their application clarified through examples.\n\n### keywords\n\nPhysical sciences > Astronomy > Cosmology \n\n### Evaluation Type\n\nEvaluation with final exam\n\n### Assessment Components\n\nExam: 100,00%\n\n### Amount of time allocated to each course unit\n\nFrequência das aulas: 42,00 hours\n**Total:**: 42,00 hours\n\n### Eligibility for exams\n\nPresence in at least 75% of the lectures.\n\n### Calculation formula of final grade\n\nThe assessment for the Cosmology lecture course consists of a final exam. The final classification in this course will be equal to the classification obtained in the final exam.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498809" . . "Presential"@en . "TRUE" . . "Data analysis in astronomy"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua._\n\n### Objectives\n\nThe general objective of this lecture course is to familiarize students with some techniques currently used in data analysis in Astronomy. In particular, it is intended that students develop an understanding of the main concepts underpinning the process of scientific inference and become capable of applying them when trying to solve problems in Astronomy.\n\n### Learning outcomes and competences\n\nIt is expected that the student will be able to apply the methods associated with the process of scientific inference to the analysis of data and the resolution of problems in Astronomy.\n\n### Working method\n\nPresencial\n\n### Program\n\n\\- Deductive and inductive inference in the scientific method. \n\\- Parameter estimation and model comparison in Physics and Astronomy: exemplification through the analysis of spectra and detection of sources. \n\\- Analytical fitting of linear physical models in the presence of Gaussian uncertainties. \n\\- Computational fitting of nonlinear physical models. \n\\- Analysis of time series and images. \n\\- Definition of experimental and observational strategies in Physics and Astronomy.\n\n### Mandatory literature\n\nP. C. Gregory; Bayesian Logical Data Analysis for the Physical Sciences, 2005 \nW. von der Linden, V. Dose, U. von Toussaint; Bayesian Probability Theory: Applications in the Physical Sciences, 2014 \n\n### Complementary Bibliography\n\nS. Andreon, B. Weaver; Bayesian Methods for the Physical Sciences, 2015 \nBailer-Jones, C.A.L.; Practical Bayesian Inference: A Primer for Physical Scientists, 2017 \nJ.M. Hilbe, R.S. de Souza and E.E.O. Ishida; Bayesian Models for Astrophysical Data, 2017 \n\n### Teaching methods and learning activities\n\nIn the theoretical-practical classes, the syllabus is explained and its application exemplified. Problems illustrating the concepts presented are also solved, and discussion is promoted in the classroom, contributing to the consolidation of knowledge and the development of a critical mind. In the practical-laboratorial classes, methods and techniques are implemented that can be used in the context of the analysis of data, such as spectra, time series and images, relevant for Physics and Astronomy.\n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nExam: 35,00%\nWritten assignment: 65,00%\n**Total:**: 100,00%\n\n### Amount of time allocated to each course unit\n\nAutonomous study: 106,00 hours\nFrequency of lectures: 56,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nIn the final exam students are required to obtain a minimum classification of 8 in 20.\n\n### Calculation formula of final grade\n\nThe final classification is given by: Nf=0.35\\*Ex+0.35\\*Tr1+0.30\\*Tr2 where Nf is the final classification (cannot be below 10 in a scale of 0 to 20), Ex is the classification in the final exam (cannot be below 8 in a scale of 0 to 20), Tr1 and Tr2 are the overall classifications respectively in the first and second pratical work tasks with written report (between 0 and 20).\n\n### Examinations or Special Assignments\n\nPratical work tasks with required submission of written reports will be given to all students, and their classification will have a weight of 65 per cent towards the final classification.\n\n### Classification improvement\n\nThe improvement of the final classification can be made only by improving the classification in the written exam, that will still have a weigh of 35 percent in the final classification. It will not be possible to improve the classification in the pratical work tasks.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498806" . . "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" . . "Extragalactic astronomy"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua._\n\n### Objectives\n\nThe aim of this course is that students acquire a thorough knowledge about different types of galaxies, their composition and the physical mechanisms responsible for the variety of observed properties and their evolution in different environments. Alongside the theoretical approach, existing observational evidence will be presented, and the major ongoing and future projects with scientific impact in this area will be mentioned.\n\n### Learning outcomes and competences\n\nIt is intended that students acquire a thorough knowledge about different types of galaxies, their composition and the physical mechanisms responsible for the variety of observed properties and their evolution in different environments. Alongside the theoretical approach, it is expected that students develop skills of reasoning and understanding, critical analysis and exposition of different results available in the literature and, if possible, experience a brief approach to research in this topic. \n\n### Working method\n\nPresencial\n\n### Program\n\nI. The Milky Way - structure, dimensions, main constituents (stars, interstellar medium, dark matter). \n \nII. Galaxy classification schemes and main properties of the different galaxy types. \n \nIII. Disks and spheroids - dynamics, total mass estimates, scaling relations and statistical properties. Star formation in disks. \n \nIV. Spectral synthesis: main types, ingredients and equations. \n \nV. Groups and clusters of galaxies: dimensions, constituents and main properties. \n \nVI. Physical mechanisms responsible for galactic evolution in groups and clusters: dynamical friction, ram-pressure stripping, tidal stripping, mergers. \n \nVII. Active galaxy nuclei - emission; different types of AGN and the unification scheme. Estimates of the mass of the central supermassive black hole. \n \nVIII. High redshift galaxies and evolutionary studies: techniques and types of distant galaxies; K and E corrections; observational biases; evolution in color, morphology, star formation rate and stellar mass function.\n\n### Mandatory literature\n\nPeter Schneider; Extragalactic Astronomy and Cosmology, Springer. ISBN: 978-3-642-54082-0/978-3-642-54083-7 (eBook) \nMo Houjun; [Galaxy formation and evolution](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000295217 \"Galaxy formation and evolution (Opens in a new window)\"). ISBN: 9780521857932 \n\n### Complementary Bibliography\n\nCarroll Bradley W.; [An introduction to modern astrophysics](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000228181 \"An introduction to modern astrophysics (Opens in a new window)\"). ISBN: 0-201-54730-9 \nB.W. Carrol, D.A. Ostlie; An Introduction to Modern Galactic Astrophysics and Cosmology, Addison-Wesley, 2007 \nSparke Linda S.; [Galaxies in the universe](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000260230 \"Galaxies in the universe (Opens in a new window)\"). ISBN: 0-521-59740-4 \nPeterson Bradley M.; [An introduction to active galactic nuclei](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000228123 \"An introduction to active galactic nuclei (Opens in a new window)\"). ISBN: 0-521-47911-8 (pbk) \nA.K. Kembhavi, J.V. Narlikar; Quasars and Active Galactic Nuclei, Cambridge University Press, 1999 \nKrolik Julian H.; [Active galactic nuclei](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000259815 \"Active galactic nuclei (Opens in a new window)\"). ISBN: 0-691-01151-6 \n\n### Comments from the literature\n\nThroughout the semester, references for scientific papers dealing with the subjects taught will be provided.\n\n### Teaching methods and learning activities\n\nClasses involve the exposure by the lecturer of the contents of the program - including the discussion of scientific results based on relevant and/or recent papers -, with the help of multimedia materials, followed by examples of application and problem solving when appropriate. \n\n### Software\n\nO trabalho prático requer conhecimentos básicos de python. \n\n### keywords\n\nPhysical sciences > Astronomy > Astrophysics \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nExam: 50,00%\nOral exam: 5,00%\nPractical assignment or project: 40,00%\nwritten assignment: 5,00%\n**Total:**: 100,00%\n\n### Amount of time allocated to each course unit\n\nAutonomous study: 120,00 hours\nFrequency of lectures: 42,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nThe exam is compulsory and has a minimum grade - see **Formula of final grade. \n \n**\n\n### Calculation formula of final grade\n\nThe assessment in this curricular unit consists of: \n\\- a final exam - which is compulsory - that contributes with a weight of 50% to the final classification; \n\\- exercises to be solved at home and presented by the students in class orally, and delivered afterwards in writing, which contribute with 10% for the final classification; \n\\- a practical assignment that contributes with 40% to the final grade. \nThe formula to compute the final classification is as follows: Nf=Ex+Q+TP where Nf is the final grade, Ex is the exam grade (rated 0-10, and required to be no less than 4/10), Q are the exercises (oral presentation + written work, rated 0 to 2) and TP is the assignment (rated 0 to 8).\n\n### Classification improvement\n\nThe improvement of the classification can be made on the written exam component only, that will still weigh 50% of the final mark.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498807" . . "Presential"@en . "TRUE" . . "The sun and the heliosphere"@en . . "6.0" . "### Teaching language\n\nEnglish\n\n### Objectives\n\nCourse that presents the main phenomena of solar activity, introduces magnetohydrodynamics (MHD) for the description of plasmas in astrophysics and provides some examples of its application to the Sun. Describes the heliosphere and presents some models for its description. Introduces and explores the concept of space weather.\n\n### Learning outcomes and competences\n\n1- To distinguish between the active and the quiet sun and to identify the main solar active phenomena associated with its magnetic field\n\n2- To use magnetohydrodynamics (MHD) as a theory to describe the behaviour of plasmas in the presence of magnetic fields\n\n3- To obtain MHD solutions for static fields and for waves in plasmas\n\n4- To use MHD in order to model the equilibrium in arcades/prominences, the energy release in solar flares via magnetic reconnection, the heating of the solar corona and the acceleration of the solar wind\n\n5- To describe the heliosphere and its main properties recognize its importance for the space weather\n\n### Working method\n\nPresencial\n\n### Program\n\n1\\. The Sun \n\\- Observations of the Sun. Solar activity. \n\\- Photosphere, transition region, chromosphere and corona. \n\\- Structure and configuration of the solar magnetic field \n \n2. The magnetohydrodynamic (MHD) description \n\\- Properties and fundamental equations \n\\- Equilibrium solutions \n\\- Waves in MHD \n \n3. Applications of MHD to the Sun \n\\- Equilibrium models for sunspots, arcades and prominences \n\\- Magnetic reconnection and solar flares. \n\\- Models for heating the solar corona. \n\\- The solar wind. models \n \n4\\. The heliosphere. \n\\- Origin and exploration \n\\- The global magnetic field of the heliosphere \n\\- Space weather \n\n### Mandatory literature\n\nEric Priest; Magnetohydrodynamics of the Sun, Cambridge University Press, 2014. ISBN: 0521854717 \nE. R. Priest; Solar Magnetohydrodynamics, Reidel Publishing Company, 2000. ISBN: 9027721386 \n\n### Complementary Bibliography\n\nAndre´ Balogh, Louis J. Lanzerotti, Steven T. Suess; The Heliosphere through the Solar Activity Cycle, Springer, 2008. ISBN: 978-3-540-74301-9 \nF. Shu; The Physics of Astrophysics. Volume 2: Gas Dynamicss, University Science Book, 1992. ISBN: 0935702652 \nL. Golub, Jay M. Pasachoff; The solar corona, Cambridge University Press, 1997. ISBN: 0521485355 \nMari Paz Miralles, Jorge Sánchez Almeida; The Sun, the Solar Wind, and the Heliosphere, Springer, 2011. ISBN: 978-90-481-9786-6 \nH. Zirin; Astrophysics of the Sun, Cambridge University Press, 1988. ISBN: 0521316073 \nMarkus J Aschwanden; Physics of the Solar Corona. An Introduction with Problems and Solutions, Springer, 2005. ISBN: 3-540-30765-6 \n\n### Teaching methods and learning activities\n\nExpository method intercalated by problem solving. Some problems will be given to students in order to be solved in classes or at home. \n \nPresentation of an article in a short talk and report, from a list provided at the beginning of the semester\n\n### keywords\n\nPhysical sciences > Astronomy > Astrophysics \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nexam: 75,00\nWritten assignment: 25,00%\n\n**Total:**: 100,00% \n\n### Amount of time allocated to each course unit\n\nAutonomous study: 120,00 hours\nFrequency of lectures: 42,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nThe student has frequency to the course if he/she misses no more than 1/4 of the planned theoretical-practical classes (TP's).\n\n### Calculation formula of final grade\n\nDistributed evaluation:\n\nFinal Mark = 25% of Mark of the Mini Test + 25% of Mark of the Talk presenting the paper and its critical analysis + 50% of Mark of the Test (to take place in 1st exam season). \n \nMinimum mark in Test: 7/20. \n \nThe Final Mark will be the mark of the normal (1st) season.\n\nIf the student has not passed, he can use the 2nd season exam for this purpose. In this case, the exam will be used as an alternative to the mini test and test components, corresponding only to 75% of the final grade. \n \nThe students with a special status, namely working-students will be subject to an evaluation equal to the remaining students. \n\n### Classification improvement\n\nIt is not allowed to improved grades on the Report/Talk presenting the paper. An improvement in the components of the Mini Test and Test is possible through an exam which counts only for 75% of the final grade.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=508145" . . "Presential"@en . "TRUE" . . "Statistical analysis and signal processing"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502172" . . "Presential"@en . "FALSE" . . "Advanced statistical physics"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509347" . . "Presential"@en . "FALSE" . . "Parallel computing"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=507411" . . "Presential"@en . "FALSE" . . "Data mining I"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=507414" . . "Presential"@en . "FALSE" . . "Partial differential equations"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502169" . . "Presential"@en . "FALSE" . . "Reflectance spectroscopy of asteroids"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509345" . . "Presential"@en . "FALSE" . . "Nonlinear physics"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509987" . . "Presential"@en . "FALSE" . . "Optical materials and devices"@en . . "6.0" . "no data" . . "Presential"@en . "FALSE" . . "Advanced quantum mechanics"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509346" . . "Presential"@en . "FALSE" . . "Computational methods applied to geophysics"@en . . "6.0" . "no data" . . "Presential"@en . "FALSE" . . "Mathematical methods in physics"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509986" . . "Presential"@en . "FALSE" . . "Mathematical modeling"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502162" . . "Presential"@en . "FALSE" . . "Petrology and geochemistry"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=499704" . . "Presential"@en . "FALSE" . . "Stochastic processes and applications"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502164" . . "Presential"@en . "FALSE" . . "Computational chemistry"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498519" . . "Presential"@en . "FALSE" . . "Measurement techniques and instrumentation"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509348" . . "Presential"@en . "FALSE" . . "Image processing and analysis"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502137" . . "Presential"@en . "FALSE" . . "Numerical analysis and simulation"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502167" . . "Presential"@en . "FALSE" . . "Data mining II"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=507421" . . "Presential"@en . "FALSE" . . "Global geology"@en . . "6.0" . "no data" . . "Presential"@en . "FALSE" . . "Statistical methods in data mining"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502139" . . "Presential"@en . "FALSE" . . "Mathematical modeling of transport phenomena"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502179" . . "Presential"@en . "FALSE" . . "Optimization"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=502765" . . "Presential"@en . "FALSE" . . "Telescopes and detectors for spatial sciences"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=507035" . . "Presential"@en . "FALSE" . . "Quantum field theory"@en . . "6.0" . "https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=509349" . . "Presential"@en . "FALSE" . . "Master in Astronomy and Astrophysics"@en . . "https://sigarra.up.pt/fcup/en/cur_geral.cur_view?pv_ano_lectivo=2022&pv_origem=cur&pv_tipo_cur_sigla=m&pv_curso_id=871" . "120"^^ . "Presential"@en . "The main objective of the Master of Astronomy is to complement and extend the training of graduate students in astronomy, physics, mathematics and related fields. In particular, in order to improve their preparation for a research career in Astronomy, through their subsequent enrolment in a Doctoral Programme in Astronomy.\n\n### Admissions Requirements\n\nApplicants to the Second Cycle (Master) in Astronomy must hold a First Cycle (Bachelor) degree (minimum of 180 ECTS credits) or equivalent (including higher education foreign degrees), whose curriculum includes at least 30 ECTS credits, or equivalent, in Mathematics and Physics, including a minimum of 12 ECTS credits in each of these scientific areas. Candidates that may verify these conditions before the end of the registration period in the Master in Astronomy can also apply. Holders of an academic, scientific or professional curriculum that is recognised as attesting the capacity to successfully complete this cycle of studies by the Scientific Committee of the Master in Astronomy may also be admitted. \n\n### Criteria for Selection and Ranking\n\nThe ranking will be done according to the following criteria and sub-criteria:\n\n* 1.1 - Academic curriculum (training area and average grade) (80%)\n * 1.1.1 - Subcriterion 1: training area (40%)\n * 1.1.2 - Subcriterion 2: average and adequacy of the degree (40%)\n* 1.2 - Scientific curriculum and professional experience (20%)\n * 1.2.1 - Subcriterion 1: technical and/or scientific publications and communications (10%)\n * 1.2.2 - Subcriterion 2: participation in research projects, internships in the area of the cycle of studies or other relevant professional experience (10%)\n\n \nNote: Candidates who do not yet hold a Bachelor's degree and/or have an academic, scientific or professional curriculum which is recognized as attesting the capacity to carry out this cycle of studies by the statutory competent scientific body, will be ranked according to the criteria and subcriteria indicated above, with the difference that the final average mark of the degree will be replaced by the weighted average mark of all curricular units completed to date. \n \n**Candidates' tiebreaker criterion:** greater number of ECTS credits obtained in the area of the cycle of studies.\n\n### Teaching Language\n\n* Fully in English\n\n### Information\n\nIt is highly desirable that candidates possess programming skills and a good written and oral command of the English language.\n\n### Contacts\n\nCourse Director: m.ast.diretor@fc.up.pt\n\nPostgraduate Section: pos.graduacao@fc.up.pt\n\nStudents: m.ast@fc.up.pt\n\n### General information\n\n* Information for applicants: https://sigarra.up.pt/fcup/en/cur_geral.cur_info_cand_view?pv_curso_id=871&pv_ano_lectivo=2022&pv_tipo_cur_sigla=m&pv_origem=cur \n\nDirector: Catarina Lobo\n\nAcronym: M:A_ASTR\n\nAcademic Degree: Master\n\nType of course/cycle of study: Masters Degree\n\nStart: 2007/2008\n\nDuration: 4 Semesters\n\n### Study Plan\n\n* Plano de Estudos oficial desde 2013/14: https://sigarra.up.pt/fcup/en/cur_geral.cur_planos_estudos_view?pv_plano_id=6001&pv_ano_lectivo=2022&pv_tipo_cur_sigla=m&pv_origem=cur \n\n* All Courses of Study: https://sigarra.up.pt/fcup/en/cur_geral.cur_planos_estudos_list?pv_curso_id=871&pv_ano_lectivo=2022&pv_tipo_cur_sigla=m&pv_origem=cur \n\n### Certificates\n\n* Master's degree in Astronomy and Astrophysics (120 ECTS credits)\n* Specialization in Astronomy and Astrophysics (66 ECTS credits)\n\n### Predominant Scientific Areas\n\n* Astronomy\n* Physics"@en . . . . "2"@en . "FALSE" . . . "Master"@en . "Thesis" . "1300.00" . "Euro"@en . "3750.00 (International) / 2250.00 (CPLP)" . "Recommended" . "* Researcher: Researchers in astronomy work on a variety of projects, from studying the formation of stars and galaxies to searching for exoplanets. They typically work in universities, research institutes, or government agencies.\n* Engineer: Engineers in astronomy develop and build instruments for astronomical observations. They also work on software for data analysis and visualization.\n* Consultant: Consultants in astronomy work with businesses and government agencies to apply astronomical knowledge to solve problems. For example, they may help to develop new technologies for space exploration or to assess the risks of asteroid impacts.\n* Science communicator: Science communicators in astronomy share the excitement of astronomy with the public through writing, public speaking, and media appearances. They may work in museums, science centers, or the media."@en . "1"^^ . "TRUE" . "Upstream"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Portuguese"@en . . "Faculdade de Ciências"@en . .