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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 ?