ISSS 2022: The different spatio-temporal scales of solar magnetism
This Web page contains links to animation complementing the set
of Lecture Notes I wrote for the International School of Space Science held
11-15 April 2022 in Università dell'Aquila, Italy.
Animations
are organized by section numbers in the Lecture notes. All are in mpeg format.
Paul Charbonneau,
Département de physique
Université de Montréal
paulchar@astro.umontreal.ca
2.3 Mean-field dynamo models
2.3.1 Linear solutions as eigenvalue problems
The left animation is an animated version of Figure 2.4;
the animation on the right uses a negative dynamo number
but is otherwise identical.
Click to launch the animation.
2.4 Flux transport dynamos
This is an animated version of Figure 2.7, see Figure caption
and accompanying text for details.
Click to launch the animation.
2.5 Babcock-Leighton models
2.5.2 A representative solution
This is an animated version of Figure 2.8, see Figure caption
and accompanying text for details.
Click to launch the animation.
2.7 Insight from MHD simulations
These is an animated version 2.12, covering one polarity reversal
of the large-scale magnetic field
in this simulation.
see Figure caption and accompanying text for details on the color-coding scheme.
Click to launch the animation.
-Last Revised 7 April 2022 by
paulchar@astro.umontreal.ca.