Abstract
This paper reviews some of the many 3D numerical experiments of the emergence
of magnetic fields from the solar interior and the subsequent interaction with the
pre-existing coronal magnetic field. The models described here are idealised, in the sense
that the internal energy equation only involves the adiabatic, Ohmic and viscous shock heating
terms. However, provided the main aim is to investigate the dynamical evolution, this
is adequate. Many interesting observational phenomena are explained by these models in a
self-consistent manner.
Original language | English |
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Pages (from-to) | 3–31 |
Number of pages | 29 |
Journal | Solar Physics |
Volume | 278 |
Issue number | 1 |
Early online date | 1 Apr 2011 |
DOIs | |
Publication status | Published - May 2012 |
Externally published | Yes |
Keywords
- Magnetohydrodynamics (MHD)
- Flux emergence
- Numerical simulation
- Solar corona