The universe is essentially composed with gas and a small amount of dust. In the interstellar medium, the average dust-to-gas ratio has an estimated value of 1% and the distribution of dust grain sizes well approximated by a power law distribution. In denser medium, such as the molecular clouds or the protostellar cores, these properties could not be true because dust dynamics is particularly affected pressure and density gradients. Most of modern studies do not consider a possible variation of dust-to-gas in these objects supposing that dust is frozen in the gas, but it is not satisfactory if its dynamics shows a complex behaviour since dust plays an important role for their thermal evolution. For that reason, I introduce the latest development of the algorithm I implemented in RAMSES that allows to treat gas and dust mixture as a monofluid in the diffusion approximation. I will present my module with the usual validation tests for dust and gas mixtures such as the dustyshock, dustywave or dustydiffusion tests and an application to protostellar collapse.
| Subject : | : | oral |
| Topics | : | Star formation |
| PDF version | : |  PDF version |
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