Changes between Version 13 and Version 14 of RadiationDriving
- Timestamp:
- 02/22/17 13:44:18 (8 years ago)
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RadiationDriving
v13 v14 13 13 $\frac{\partial E}{\partial t}+\nabla\cdot\left[\left(E+P\right)\mathbf{u}\right]=\mathbf{f}_{rad}\cdot\mathbf{u}$ 14 14 15 We average the radiation flux over the azimutal angle ($2\pi$) and divide the polar angle ($\pi$) into n small subdivision. The default is $n=30$ and you can change it in physics/physics_declarations.f90 DustSublimationRadius=30. The radiation will be aborsbed by the gas and dust by opacity. In our paper, opacity can be a function of distance to the luminous object. You can checkout source/radforce.f90 Kappa_try(pos). 15 Basically, this 2D ray tracing is a part of 2D sampling diagram function which already exist in AstroBEAR. We use CreatePDF() subroutine to create a 2D empty table (please see processings/pdfs.f90). The 2D table will associate two variables, say x,y and give a function of f(x,y). In 2D ray tracing algorithm, x is the polar angle theta, and y is the distance to the luminous object, f will be the flux intensity. We average the radiation flux over the azimutal angle ($2\pi$) and divide the polar angle ($\pi$) into n small subdivision (call it column afterwards). The default is $n=30$ and you can change it in physics/physics_declarations.f90 DustSublimationRadius=30. Each column should be further divided into m to carry out the ray tracing algorithm. You need to add this number m in your problem module. 16 17 The radiation will be aborsbed by the gas and dust by opacity. In our paper, opacity can be a function of distance to the luminous object. You can checkout source/radforce.f90 Kappa_try(pos). 16 18 17 19 $\frac{d I}{d x}=-\kappa I$