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In Smoothed Particle Hydrodynamical (SPH) simulations of star formation a simple barotropic equation of state is normally used in every situation. However, in practice this is not realistic because it does not take account of the thermal history of a protostar and is unable to capture thermal inertia effects. Stamatellos et al. (2007) have introduced a new algorithm for treating the thermal and radiative effects influencing the energy equation. This algorithm captures the trapping of cooling radiation, opacity changes and internal energy changes due to H2, H and He. I will present SPH simulations of the collapse and fragmentation of low-mass low-turbulence cores, and quantify the difference between simulations performed using a barotropic equation of state and simulations which treat the energy equation and associated radiation transport. Further to this I will present models of the prestellar cores in Rho Ophiuchus using initial conditions constrained by the observations. I will compare the resulting mass function, the multiplicity statistics and the kinematics of these cores with observations of existing young stellar objects in Rho Ophiuchus.
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