State of the art single fluid MHD numerical modeling of the coupled solar atmosphere
Abstract
Modeling the solar atmosphere has for a long time been known to be a very complex problem. The wealth of observational features identified in solar observations have multiplied with increasing spatial, temporal and spectral resolution. To explain the high quality of space and ground based observations, models must be very sophisticated and be able to treat a number of physical regimes, where the dominating terms in the equations change drastically. Numerical simulations are now able to explain some, but certainly not all of the observed features. The numerical complexity of solving the equations governing the physics of the solar atmosphere is very high, and a number of different numerical techniques must be used in order to create a coherent picture of the connected solar atmosphere. We are now at a level where simulations have to include a much larger range in vertical extend than has been previously done. The wealth of numerical problems arising when doing so has lead to a number of numerical codes that are specialized to deal with a specific problem, and which now are being augmented to handle a larger range of problems. Hopefully with time we will have a number of numerical codes that are sophisticated enough to deal reliably with the whole solar atmosphere. I will give a review of some the codes that have been able to produce results from a fully connected solar model.
- Publication:
-
SDO-4: Dynamics and Energetics of the Coupled Solar Atmosphere. The Synergy Between State-of-the-Art Observations and Numerical Simulations
- Pub Date:
- March 2012
- Bibcode:
- 2012decs.confE.115G
- Keywords:
-
- SDO;
- SDO-4;
- SDO 4;
- SDO Workshop;
- SDO-4/IRIS/Hinode Workshop;
- Solar Dynamic Observatory