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PX420 Solar Magnetohydrodynamics

The moodle page is www.warwick.ac.uk/px420

Valery Nakariakov

The solar corona observed in EUV from space with SOHO/EIT.

Aims:

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.

Objectives:

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

Syllabus:

  1. An outline of observational properties ranging from the solar interior ot the Sun's outer atmosphere
  2. Theoretical aspects of solar magnetohydrodynamics (MHD)
  3. Magnetic equilibria. Stratification. Force-free magnetic fields. Magnetic arcades, prominences, suspots, intense flux tubes.
  4. MHD Waves. Helioseismology.
  5. Solar flares. Heating of the solar corona. Coronal mass ejections and space weather.

Commitment: 15 Lectures

Assessment: 1.5 hour examination

Recommended Texts:

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.

Leads from: PX264 Introduction to Fluids and PX392 Plasma Electrodynamics