1. Modelling of 2D radiative transfer in quiescent prominences

2. Structure of the presentation
Modelling of prominences
Grid of models
Contribution functions
Results and analyses
Conclusion

3. Two dimensional Kippenhahn-Schlüter model

4. Two dimensional Kippenhahn-Schlüter model

5. Kuperus-Raadu model

6. 2D radiative transfer equation

7. Modelling of 2D radiative transfer in quiescent prominences
Heasley a Mihalas (1976) – non-LTE model with inclusion of MHS and radiative transfer
Mihalas et al. (1978) – the first 2D model
Heinzel et al. (1987) – inclusion of PRD
Fontenla et al. (1996) – multi-threat model
Anzer a Heinzel (1999) – inclusion of PCTR
Heinzel a Anzer (2001) – generalisation of MHS for 2D

8. 2D models of the quiescent prominences
Motivation – the different orientation of the magnetic field lines towards the observer (Heinzel et al. 2001)
Model – 12-level Hydrogen atom
– MHS equations of 2D K-S type
– numerical solution of radiative transfer by ALI method
(Auer and Paletou 1994) with usage of SC (Kunasz and Auer 1988)

9. Short Characteristics method (SC)

10. Two-dimensional magnetic dip model

11. The temperature structure

12. The magnetic dip
The density structure

13. Grid of models
Constant parameters

14. The geometrical shape of the prominence threats of each model

15. The dependence of profiles on magnetic field orientation

16. Contribution functions

17. Contribution functions – A1 Lb

19. Conclusion Multi-threat model Inclusion of the velocity field
Creation of 3D code
Comparison of synthetic profiles with observed profiles on SOHO

20. Who says that Solar Physics is boring ?