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The solar corona observed in EUV from space with SOHO/EIT.
To review the basic physics underlying the structure and the dynamics of the sun, to provide a background in the description of physical processes in the Sun in terms of magnetohydrodynamics and to show the results of recent observations.
At the end of this module you should:
- Know the structure of the Sun and the main features and phenomena observed on the solar surface and in the solar atmosphere
- Understand the basic physical processes at work in the sun
- Be able to describe the basic dynamic processes operating in the Sun, in terms of MHD
- An outline of observational properties ranging from the solar interior ot the Sun's outer atmosphere
- Theoretical aspects of solar magnetohydrodynamics (MHD)
- Magnetic equilibria. Stratification. Force-free magnetic fields. Magnetic arcades, prominences, suspots, intense flux tubes.
- MHD Waves. Helioseismology.
- Solar flares. Heating of the solar corona. Coronal mass ejections and space weather.
Commitment: 15 Lectures
Assessment: 1.5 hour examination
Priest, E.R., Solar Magnetohydrodynamics, Reidel, 1982
Priest, E.R., Magnetohydrodynamics of the Sun, Cambridge University Press, 2014
Golub, L. and Pasachoff, J.M., Nearest Star: The Surprising Science of Our Sun, Harvard University Press, 2001
Aschwanden, M.J., Physics of the Solar Corona, Springer-Praxis 2004.