Abstract
The study of radiatively driven winds in O and B stars has been achieved mainly through analytic solutions of the equation of motion. These solutions can only be applied to simple geometries. Presented here are preliminary results of a particle based Lagrangian code (applied to a simple 1D radiatively driven wind test case), which will be able to resolve structure down to the smallest scales without becoming temporally prohibitive. This approach to modelling radiatively driven winds can be applied to the dispersal of massive young stellar objects' natal circumstellar material, Be star wind structure and CV disc winds.
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Porter, J.M. Radiatively driven winds using Lagrangian hydrodynamics. Astrophys Space Sci 216, 93–94 (1994). https://doi.org/10.1007/BF00982473
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DOI: https://doi.org/10.1007/BF00982473