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Forming stars emit a significant amount of radiation into their natalenvironment. While the importance of radiation feedback from high-mass stars iswidely accepted, radiation has generally been ignored in simulations oflow-mass star formation. I use ORION, an adaptive mesh refinement (AMR)three-dimensional gravito-radiation-hydrodynamics code, to model low-mass starformation in a turbulent molecular cloud. I demonstrate that includingradiation feedback has a profound effect on fragmentation and protostellarmultiplicity. Although heating is mainly confined within the core envelope, itis sufficient to suppress disk fragmentation that would otherwise result inlow-mass companions or brown dwarfs. As a consequence, turbulent fragmentation,not disk fragmentation, is likely the origin of low-mass binaries.

The Effects of Radiation Feedback on Early Fragmentation and Multiplicity