. "Climate Change"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Solar physics and space weather"@en . . "6" . "Specific Competition\nCE1 - Understand the basic conceptual schemes of Astrophysics\nCE2 - Understand the structure and evolution of stars\nCE10 - Use current scientific instrumentation (both Earth-based and Space-based) and learn about its innovative technologies.\nGeneral Competencies\nCG2 - Understand the technologies associated with observation in Astrophysics and instrumentation design\nCG4 - Evaluate the orders of magnitude and develop a clear perception of physically different situations that show analogies allowing the use, to new problems, of synergies and known solutions\nBasic skills\nCB6 - Possess and understand knowledge that provides a basis or opportunity to be original in the development and/or application of ideas, often in a research context\nCB7 - That students know how to apply the knowledge acquired and their ability to solve problems in new or little-known environments within broader contexts\nCB8 - That students are able to integrate knowledge and face the complexity of formulating judgments based on information that, being incomplete or limited, includes reflections on the social and ethical responsibilities linked to the application of their knowledge and judgments\nCB10 - That students possess the learning skills that allow them to continue studying in a way that will be largely self-directed or autonomous\nExclusive to the Theory and Computing Specialty\nCX6 - Understand the structure of the Sun, its evolution and magnetic activity\n6. Subject contents\nTheoretical and practical contents of the subject\n-------------------------------------------------- -----------------------------------------------\nFirst part: Solar interior\n---------------------------------------------------------------- -------------------------------------------------\n\nTopic 1. Global properties of the Sun\n \nTopic 2. Solar interior \n \n2.1 Models of stellar interior. Nuclear reactions\n2.2 Controversy of solar neutrinos\n2.3 The standard model of the solar interior\n\nTopic 3. Helioseismology\n\n3.1 Waves in isothermal and non-isothermal fluids, with and without gravity\n3.2 Formation of stationary modes in the Sun: pyg modes\n3.3 Review of inversion methods seismology to recover the properties of the solar interior\n\nTopic 4. Convection and oscillations: theoretical aspects and simulations\n \n4.1 Convection and granulation: numerical simulations of convection\n4.2 Supergranulation, mesogranulation, giant cells. Explanation of the various scales\n4.3 Generation of sound waves. Vorticity generation\n4.4 Shape of spectral lines in convection models\n \n-------------------------------------- --------------------\nSecond part: Photosphere and chromosphere\n-------------------- ----------------------------------\n\nTopic 5. Radiative transport of polarized light\n \n5.1 Radiative transport\n 5.1.1 Zeeman effect \n 5.1.2 Transport equation for polarized light\n \nTopic 6. Photospheric magnetism\n6.1 Photospheric magnetic structures: Spots, pores, faculae, photospheric network and calm Sun\n6.2 MHD equations. Concentration of the field by convective movements, inhibition of convection by strong fields, magnetoconvection, potential and free force fields 6.3 Convective\ncollapse, field buoyancy, field expansion with height, Wilson depression, Evershed effect by hot tube buoyancy\n6.4 Simulations Numerical measurements of magnetoconvection in strong and weak fields. Explanation of the photospheric magnetic structures in terms of MHD and MHS\n6.5 Emergency simulations of magnetic flux and simulations of spots, threshold points and the penumbra\n\nTopic 7. Chromospheric magnetism\n \n7.1 Spicules, filaments and protuberances. Structure, balance and dynamics\n7.2 MHD waves. Magneto-acoustic waves and Alfvén. Phase speed. Relationship between the disturbed magnitudes\n7.3 Transformation of modes by stratification. Fast mode refraction\n7.4 Mode transformation by 3D stratification. Alfvén mode transformation. Angle dependence\n7.5 Observational evidence of mode transformation in solar magnetized plasma. Ramp effect. Fast and slow modes in one spot. Slow propagation in spots towards the crown\n7.6 Acoustic halos. Periodicity of waves observed in umbras and penumbras of sunspots\n7.7 Mechanisms of heating of the chromosphere \n\nTopic 8. Solar rotation, dynamo and solar cycle \n\n8.1 Solar rotation \n8.2 Solar dynamo. Parker's model of oscillatory alpha-omega dynamo, mean field models\n8.3 Solar cycle and its observational properties\n8.4 Numerical models of differential rotation and solar dynamo. \n8.5 Cycle predictions. Maunder Minimum\n \n----------------------------------------------- --------------------------------\nPart Three: The Corona, Heliosphere, and Space Weather\n------- -------------------------------------------------- ----------------------\n\nTopic 9. The solar corona\n\n9.1 Observations: X-ray and EUV space missions\n9.2 Theory: strongly magnetized and hot plasma, highly conductive and optically thin\n9.3 Radiative transport in optically thin plasmas: radiative cooling\n9.4 Equilibrium structures, coronal loops and magnetic extrapolation\n9.5 Eruptive phenomena: solar flares. CSHKP model\n9.6 Eruptive phenomena: coronal mass ejections (CME)\n9.7 The problem of coronal heating: the tirade waves against reconnection\n\nTopic 10. Space weather\n\n10.1 The solar wind and the heliosphere\n10.2 The Earth's magnetosphere: general structure. Magnetospheric space missions\n10.3 Solar storms: summary of physical properties. Impact on society\n10.4 The physics of solar storms: impact of CMEs on the magnetosphere\n10.5 Reconnection in the magnetopause and in the magnetic tail. NASA's MMS mission. auroras" . . "Presential"@en . "FALSE" . . "Master in Astrophysics"@en . . "https://www.ull.es/en/masters/astrophysics/" . "90"^^ . "Presential"@en . "The exceptional atmospheric conditions for top-quality astronomic observation to be found in the Canary Islands, together with its geographic proximity and excellent connections with Europe, justify the presence here of the European Northern Hemisphere Observatory (ENO). This fact, along with the consequent concentration of teachers and researchers around the Canary Island Institute of Astrophysics, the ULL Department of Astrophysics and the Observatories, generates the ideal atmosphere for a Master in Astrophysics in which direct contact with leading professionals represents exceptional value added. The Master has been designed based on an ample and rigorous choice of subjects, options and itineraries that that take the form of three specialities: “Theory and Computing Speciality”, “Observation and Instrumentation Speciality” and “Material Structure”\n\nGeneral skills\nKnow the advanced mathematical and numerical techniques that allow Physics and Astrophysics to be applied to solving complex problems using simple models\nUnderstand the technologies associated with observation in Astrophysics and the design of instrumentation\nAnalyse a problem, study the possible solutions published and propose new solutions or lines of attack\nAssess orders of magnitude and develop a clear perception of physically different situations that show analogies allowing the use of synergies and known solutions for new problems\nSpecific skills\nUnderstand the basic conceptual schemes of Astrophysics\nUnderstand the structure and evolution of the stars\nUnderstand the mechanisms of nucleosynthesis\nUnderstand the structure and evolution of galaxies\nUnderstand the models of the origin and evolution of the Universe\nUnderstand the structure of matter to be able to solve problems related to the interaction between matter and radiation in different energy ranges\nKnow how to find solutions to specific astrophysical problems on your own, using specific bibliography with minimum supervision\nKnow how to work independently on new research projects\nKnow how to programme, at least in one important language for scientific calculation in Astrophysics\nUnderstand the instrumentation used to observe the universe in the different frequency ranges\nUse current scientific instrumentation (both Earth-based and Space-based) and have a command of their innovative technologies\nKnow how to use current astrophysical instrumentation (both in terrestrial and space observatories), especially the instrumentation that uses the most innovative technology and know the foundations of the technology used\nApply the knowledge acquired to undertake an original research work in Astrophysics"@en . . . "1.5"@en . "FALSE" . . . "Master"@en . "Thesis" . "Not informative" . "no data"@en . "Not informative" . "None" . "no data"@en . "no data" . "FALSE" . "Upstream"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .