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1.1.3 Source regions of the heliospheric magnetic field
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- Probe fine-scale structure of the solar photosphere, including waves and the emergence, evolution and dynamics of magnetic flux.
- Uncover the effects of waves and magnetic field changes on the upper atmospheric layers (e.g. production of transient events (Galsgaard et al., 2005)).
- Study of the magnetic fields at the poles of the Sun. [high latitude]
- Origin of the spicules and other chromospheric features (De Pontieu et al., 2004). Polar spicules (Johannesson and Zirin, 1996).
- How does the Sun’s magnetic field link into space?
- How does the Sun’s magnetic field change over time? [multiple orbits]
- Measure how the polarity and large scale structures of the Sun’s magnetic field in interplanetary space varies close to the Sun as it moves from solar minimum towards maximum and the global field reverses.
- Link changes in solar magnetic field with changes in energy input into the solar wind.
- How does the Sun’s magnetic field change over time? [multiple orbits]
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- Understand what determines the amount of open flux from the Sun, how open field lines are distributed at the solar surface at any given time, and how these open field lines reconnect and change their connection across the solar surface in time. [perihelion]
- Measure the outflow velocity maps of the solar wind in the outer corona to identify static and dynamic regions. (This is rather an activity to be linked to one or more objectives).
- Origin of the open magnetic flux from:
- Coronal holes.
- Active regions.
- Quiet Sun.
- Loops of varying heights.
- Tips and legs of the helmet streamer.
- Polar plumes.
- Other solar structures.
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