Solar physics and space weather
Specific Competition
CE1 - Understand the basic conceptual schemes of Astrophysics
CE2 - Understand the structure and evolution of stars
CE10 - Use current scientific instrumentation (both Earth-based and Space-based) and learn about its innovative technologies.
General Competencies
CG2 - Understand the technologies associated with observation in Astrophysics and instrumentation design
CG4 - 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
Basic skills
CB6 - 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
CB7 - That students know how to apply the knowledge acquired and their ability to solve problems in new or little-known environments within broader contexts
CB8 - 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
CB10 - That students possess the learning skills that allow them to continue studying in a way that will be largely self-directed or autonomous
Exclusive to the Theory and Computing Specialty
CX6 - Understand the structure of the Sun, its evolution and magnetic activity
6. Subject contents
Theoretical and practical contents of the subject
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First part: Solar interior
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Topic 1. Global properties of the Sun
Topic 2. Solar interior
2.1 Models of stellar interior. Nuclear reactions
2.2 Controversy of solar neutrinos
2.3 The standard model of the solar interior
Topic 3. Helioseismology
3.1 Waves in isothermal and non-isothermal fluids, with and without gravity
3.2 Formation of stationary modes in the Sun: pyg modes
3.3 Review of inversion methods seismology to recover the properties of the solar interior
Topic 4. Convection and oscillations: theoretical aspects and simulations
4.1 Convection and granulation: numerical simulations of convection
4.2 Supergranulation, mesogranulation, giant cells. Explanation of the various scales
4.3 Generation of sound waves. Vorticity generation
4.4 Shape of spectral lines in convection models
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Second part: Photosphere and chromosphere
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Topic 5. Radiative transport of polarized light
5.1 Radiative transport
5.1.1 Zeeman effect
5.1.2 Transport equation for polarized light
Topic 6. Photospheric magnetism
6.1 Photospheric magnetic structures: Spots, pores, faculae, photospheric network and calm Sun
6.2 MHD equations. Concentration of the field by convective movements, inhibition of convection by strong fields, magnetoconvection, potential and free force fields 6.3 Convective
collapse, field buoyancy, field expansion with height, Wilson depression, Evershed effect by hot tube buoyancy
6.4 Simulations Numerical measurements of magnetoconvection in strong and weak fields. Explanation of the photospheric magnetic structures in terms of MHD and MHS
6.5 Emergency simulations of magnetic flux and simulations of spots, threshold points and the penumbra
Topic 7. Chromospheric magnetism
7.1 Spicules, filaments and protuberances. Structure, balance and dynamics
7.2 MHD waves. Magneto-acoustic waves and Alfvén. Phase speed. Relationship between the disturbed magnitudes
7.3 Transformation of modes by stratification. Fast mode refraction
7.4 Mode transformation by 3D stratification. Alfvén mode transformation. Angle dependence
7.5 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
7.6 Acoustic halos. Periodicity of waves observed in umbras and penumbras of sunspots
7.7 Mechanisms of heating of the chromosphere
Topic 8. Solar rotation, dynamo and solar cycle
8.1 Solar rotation
8.2 Solar dynamo. Parker's model of oscillatory alpha-omega dynamo, mean field models
8.3 Solar cycle and its observational properties
8.4 Numerical models of differential rotation and solar dynamo.
8.5 Cycle predictions. Maunder Minimum
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Part Three: The Corona, Heliosphere, and Space Weather
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Topic 9. The solar corona
9.1 Observations: X-ray and EUV space missions
9.2 Theory: strongly magnetized and hot plasma, highly conductive and optically thin
9.3 Radiative transport in optically thin plasmas: radiative cooling
9.4 Equilibrium structures, coronal loops and magnetic extrapolation
9.5 Eruptive phenomena: solar flares. CSHKP model
9.6 Eruptive phenomena: coronal mass ejections (CME)
9.7 The problem of coronal heating: the tirade waves against reconnection
Topic 10. Space weather
10.1 The solar wind and the heliosphere
10.2 The Earth's magnetosphere: general structure. Magnetospheric space missions
10.3 Solar storms: summary of physical properties. Impact on society
10.4 The physics of solar storms: impact of CMEs on the magnetosphere
10.5 Reconnection in the magnetopause and in the magnetic tail. NASA's MMS mission. auroras
Presential
FALSE
Solar physics and space weather
Funded by the European Union. Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or HaDEA. Neither the European Union nor the granting authority can be held responsible for them. The statements made herein do not necessarily have the consent or agreement of the ASTRAIOS Consortium. These represent the opinion and findings of the author(s).
