Titlebook: Computational Methods in Transport; Granlibakken 2004 Frank Graziani Conference proceedings 2006 Springer-Verlag Berlin Heidelberg 2006 App

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https://doi.org/10.1007/978-3-319-22759-7ave (and will ever have) about distant objects (exceptions are detected neutrinos from the Sun and supernova SN1987a, and in a near future the gravitational waves). However, there is an even more compelling reason for the a need to deal with detailed radiation transport in astrophysics: In many astr

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Marco Hübner,Philipp Jahn,Gregor Tewaaggime. We consider the non-relativistic regime to be characterized by material velocities less than or equal to one percent of the speed of light. In most applications, the radiative transfer equations are coupled to the hydrodynamics equations. We first describe a radiation-hydrodynamics model that

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Advances in Production Technologycludes the mean-free-path, one can use an effective propagation kernel that will necessarily be sub-exponential. We come to this conclusion using both standard transport theory for variable media and a point-process approach developed recently by A. Kostinski. The ramifications of this finding for m

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Wolfgang Schulz,Toufik Al Khawlich as Monte Carlo [12], or SHDOM [3]. However, it is usually required too much time to make a simulation which is inconvenient when just we need an answer on a simple question like how significant the 3D effects are for a given problem. The perturbation method is what comes to mind first if we need

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https://doi.org/10.1007/978-3-319-12304-2f four possible canopy reflectance models. The overview is followed by the description of the . coupled leaf/canopy turbid medium reflectance model based on natural averaging. The model follows conventional radiative transfer theory with modification for canopy architecture as characterized by leaf