Non-equilibrium ionization in 3D numerical models
Abstract
The dynamic timescales in the chromosphere and transition region have been observed to be much smaller then the ionization equilibration timescales of many ions found in the region. Due to the fast changes in the properties of the atmosphere, long ionization- and recombination times may lead to ions being found far from their equilibrium temperatures. Spectroscopic investigations therefore needs to be interpreted with the help of numerical modeling in order to produce reliable results. By solving the rate equations within a realistic MHD simulation of the solar atmosphere, we are able to follow the ionization balance, and study the non equilibrium effects of the emitting gas. Due top lack of computation power, this has previously been done in simple 1D, but because of the many free parameters in these models, their conclusions are not free of uncertainties. The resent development in computing technology and atmospheric modeling makes it possible to study the full 3D effect of non equilibrium ionization. With the solar atmosphere model Bifrost, we have a 3D platform for calculating and following the ionization degree of important atoms of high abundances in the solar atmosphere. We will present our implementation, and a study of the carbon IV 1549 Å , Iron XII 195 Å, Oxygen IV 1399 Å and 1401 Å lines in 2D.
- 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.118O
- Keywords:
-
- SDO;
- SDO-4;
- SDO 4;
- SDO Workshop;
- SDO-4/IRIS/Hinode Workshop;
- Solar Dynamic Observatory