The Equations of Radiation Hydrodynamics
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چکیده
In astrophysical flows, radiation often contains a large fraction of the energy density, momentum density, and stress (i.e., pressure) in the radiating fluid. Furthermore, radiative transfer is usually the most effective energy-exchange mechanism within the fluid. To describe the behavior of such flows we need conservation laws that account accurately for both the material and the radiative contributions to the flow dynamics. To estilmate the importance of radiation in fixing the local properties of a radiating fluid, consider the ratio R of the material internal energy density 2 to the radiation energy density E; for a perfect gas and equil ib rium radiation
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تاریخ انتشار 1997