12/28/2023 0 Comments Core animator 1.4![]() We analyse the evolution and properties of a large sample of protostellar discs formed in a radiation hydrodynamical simulation of star cluster formation.ĭue to the chaotic nature of the star formation process, we find an enormous diversity of young protostellar discs, including misaligned discs, and discs whose orientations vary with time. We present results from the first population synthesis study of protostellar discs. On the diversity and statistical properties of protostellar discs (2018) ![]() It is found that close binary systems are more frequent at lower metallicity, due to enhanced cooling and fragmentation on small spatial scales. For the first time, these calculations treat separate gas and dust temperatures and include a model for the diffuse interstellar medium and a simple chemical model. Radiation hydrodynamical simulations of star formation in a 500 solar-mass molecular cloud with different metallicities, ranging from 1/100 to 3 times solar metallicity. The dependence of stellar properties on metallicity (2019) Thus, the grain size distribution can vary substantially in the first core/pre-stellar disc even at these very early times. In gravitationally-unstable discs, grain growth is more rapid in the spiral density waves leading to the larger grains being preferentially found in the spiral waves even though there is no migration of grains relative to the gas. Once the first hydrostatic core forms rapid dust growth to sizes in excess of 100 micron occurs within the core (before stellar core formation), with larger grains closer to the centre of the core. We begin with a typical interstellar dust grain size distribution and study dust growth during the collapse of a molecular cloud core and the evolution of the first hydrostatic core, prior to the formation of the stellar core. We present results from the first study of dust grain growth during the earliest phases of star formation using three-dimensional hydrodynamical simulations. Dust coagulation during the early stages of star formation: molecular cloud collapse and first hydrostatic core evolution
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