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The early evolution of massive discs have been studied in detail using simple cooling parameters to describe the thermodynamics and by using grid-based radiative transfer calculations. We will present new results from simulations using a Smoothed Particle Hydrodynamics code with radiative transfer, to follow the advancement of gravitationally unstable discs surrounding young stars. Such discs may soon be observable using ALMA. The radiative transfer is treated using an implicit flux-limited diffusion approach. We consider a variety of initial conditions and the effect of changing the dust opacity on the disc's evolution and compare our results with previous work.
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