Influence of protostellar outflows on star and protoplanetary disk formation in a massive star-forming clump

TL;DR

Protostellar outflows significantly influence star and disk formation in massive star-forming regions by affecting temperature, accretion, and fragmentation, thus shaping the stellar population.

Contribution

This study presents the first magnetohydrodynamics simulation of massive star-forming clumps including ambipolar diffusion, radiative transfer, and outflows, systematically comparing with models without outflows.

Findings

Outflows add kinetic energy and impact temperatures in the clump and disks.

Outflows reduce accretion rates onto protostars.

Outflows promote increased fragmentation and a more numerous stellar population.

Abstract

Context. Due to the presence of magnetic fields, protostellar jets/outflows are a natural consequence of accretion onto protostars. They are expected to play an important role for star and protoplanetary disk formation. Aims. We aim to determine the influence of outflows on star and protoplanetary disk formation in star forming clumps. Methods. Using RAMSES, we perform the first magnetohydrodynamics calculation of massive star-forming clumps with ambipolar diffusion, radiative transfer including the radiative feedback of protostars and protostellar outflows while systematically resolving the disk scales. We compare it to a model without outflows. Results. We find that protostellar outflows have a significant impact on both star and disk formation. They provide significant additional kinetic energy to the clump, with typical velocities of a few 10 km/s, impact the clump and disk temperatures, reduce the accretion rate onto the protostars and enhance fragmentation in the filaments. We find that they promote a more numerous stellar population. They do not impact much the low mass end of the IMF, which is probably controlled by the mass of the first Larson core, however, that they have an influence on its peak and high-mass end. Conclusions. Protostellar outflows appear to have a significant influence on both star and disk formation and should therefore be included in realistic simulations of star-forming environments.