Sink particle radiative feedback in smoothed particle hydrodynamics models of star formation

Abstract

We present a new method for including radiative feedback from sink particles in smoothed particle hydrodynamics simulations of low-mass star formation, and investigate its effects on the formation of small stellar groups. We find that including radiative feedback from sink particles suppresses fragmentation even further than calculations that only include radiative transfer within the gas. This reduces the star-formation rate following the formation of the initial protostars, leading to fewer objects being produced and a lower total stellar mass. The luminosities of sink particles vary due to changes in the accretion rate driven by the dynamics of the cluster gas, leading to different luminosities for protostars of similar mass. Including feedback from sinks also raises the median stellar mass. The median masses of the groups are higher than typically observed values. This may be due to the lack of dynamical interactions and ejections in small groups of protostars compared to those that occur in richer groups. We also find that the temperature distributions in our calculations are in qualitative agreement with recent observations of protostellar heating in Galactic star-forming regions.

Accepted for publication in MNRAS, 18 pages, 12 figures

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Cited by in corpus (13)

• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. A Statistical Characterization of Class 0 and I Protostellar Disks
• STARFORGE: Toward a comprehensive numerical model of star cluster formation and feedback
• The statistical properties of stars and their dependence on metallicity
• There is no magnetic braking catastrophe: Low-mass star cluster and protostellar disc formation with non-ideal magnetohydrodynamics
• Atomic and molecular gas from the epoch of reionization down to redshift 2
• The role of the H${}_2$ adiabatic index in the formation of the first stars
• The statistical properties of stars at redshift, z=5, compared with the present epoch
• Variation of the low-mass end of the stellar initial mass function with redshift and metallicity
• The statistical properties of protostellar discs and their dependence on metallicity
• The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency
• Insights into the first and second hydrostatic core stages from numerical simulations
• Numerical Methods for Simulating Star Formation
• Grouped star formation: converting sink particles to stars in hydrodynamical simulations