On the origin of the peak of the stellar initial mass function: exploring the tidal screening theory

Abstract

Classical theories for the stellar initial mass function (IMF) predict a peak mass which scales with the properties of the molecular cloud. In this work, we explore a new theory proposed by Lee & Hennebelle (2018). The idea is that the tidal field around first Larson cores prevents the formation of other collapsing clumps within a certain radius. The protostar can then freely accrete the gas within this radius. This leads to a peak mass of roughly $10M_{1LC}$, independent of the parent cloud properties. Using simple analytical arguments, we derive a collapse condition for clumps located close to a protostar. We then study the tidal field and the corresponding collapse condition using a series of numerical simulations. We find that the tidal field around protostars is indeed strong enough to prevent clumps from collapsing unless they have high enough densities. For each newly formed protostar, we determine the region in which tidal screening is dominant. We call this the tidal bubble. The mass within this bubble is our estimate for the final mass of the star. Using this formalism, we are able to construct a very good prediction for the final IMF in our simulations. Not only do we correctly predict the peak, but we are also able to reproduced the high and low mass end of the IMF. We conclude that tidal forces are important in determining the final mass of a star and might be the dominant effect in setting the peak mass of the IMF.

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Cited by in corpus (14)

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• Effects of the environment and feedback physics on the initial mass function of stars in the STARFORGE simulations
• The Origin of the Stellar Mass Distribution and Multiplicity
• What is the role of stellar radiative feedback in setting the stellar mass spectrum?
• The IMF and multiplicity of stars from gravity, turbulence, magnetic fields, radiation and outflow feedback
• Can magnetized turbulence set the mass scale of stars?
• Photometric, kinematic and variability study in the young open cluster NGC 1960
• How magnetic field and stellar radiative feedback influences the collapse and the stellar mass spectrum of a massive star forming clump
• The effect of tidal forces on the Jeans instability criterion in star-forming regions
• The influence of the cloud virial parameter on the initial mass function
• Do tides play a role in the determination of the pre-stellar core mass function?
• On the Jeans criterion for hydrostatic and infalling gas
• When did the initial mass function become bottom-heavy?