Abstract
Abstract Unlike the Sun, most observed stars are part of a multiple star system, but the formation of such systems is still not well understood. To study this problem, we utilize a run from the STARFORGE simulation suite that simulates the evolution of star-forming Giant Molecular Clouds (GMCs). The run starts with a GMC of an initial mass of 2 × 104 M ⊙ and takes gravity, magneto-hydrodynamics and non-isothermal thermodynamics into account. The simulation also includes stellar feedback in the forms of radiation and protostellar jets, where the radiation field is explicitly evolved. In this note, we discuss the orbital period, semimajor axis, multiplicity fraction, and multiplicity frequency distributions, and compare these with observations. We find good agreement with the observed multiplicity fractions but also find a deficit of mass ratios close to unity and close companions, which we attribute to the lack of resolved disks in our simulation.
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