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

TL;DR

This paper proposes a new tidal screening theory for the stellar initial mass function (IMF) peak, demonstrating through simulations that tidal forces around protostars regulate accretion and shape the IMF independently of cloud properties.

Contribution

The study introduces a novel tidal screening model that accurately predicts the IMF peak and its shape, emphasizing the role of tidal forces in star formation.

Findings

Tidal fields prevent collapse of low-density clumps near protostars.

The tidal bubble concept predicts the final stellar mass effectively.

The model reproduces the entire IMF, including peak and high/low mass ends.

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 $10 \, M_{\mathrm{1LC}}$, 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.