Modelling of 2D radiative transfer in quiescent prominences

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

Two dimensional Kippenhahn-Schlüter model

Two dimensional Kippenhahn-Schlüter model

Kuperus-Raadu model

2D radiative transfer equation

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

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)

Short Characteristics method (SC)

Two-dimensional magnetic dip model

The temperature structure

The magnetic dip The density structure

Grid of models Constant parameters

The geometrical shape of the prominence threats of each model

The dependence of profiles on magnetic field orientation

Contribution functions

Contribution functions – A1 Lb

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

Who says that Solar Physics is boring ?