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We investigate the effect of heating by luminosity sources in a simulation ofclustered star formation. Our heating method involves a simplified continuumradiative transfer method that calculates the dust temperature. The gastemperature is set by the dust temperature. We present the results of foursimulations, two simulations assume an isothermal equation of state and the twoother simulations include dust heating. We investigate two mass regimes, i.e.,84 Msun and 671 Msun, using these two different energetics algorithms. The massfunctions for the isothermal simulations and simulations which include dustheating are drastically different. In the isothermal simulation, we do not formany objects with masses above 1 Msun. However, the simulation with dustheating, while missing some of the low-mass objects, forms high-mass objects(~20 Msun) which have a distribution similar to the Salpeter IMF. The envelopedensity profiles around the stars formed in our simulation match observedvalues around isolated, low-mass star-forming cores. We find the accretionrates to be highly variable and, on average, increasing with final stellarmass. By including radiative feedback from stars in a cluster-scale simulation,we have determined that it is a very important effect which drastically affectsthe mass function and yields important insights into the formation of massivestars.

Fragmentation and Evolution of Molecular Clouds. II: The Effect of Dust Heating