Analytical star formation rate from gravoturbulent fragmentation

TL;DR

This paper introduces an analytical model for star formation rates in molecular clouds that accounts for turbulence and density variations, aligning well with observations and eliminating the need for arbitrary thresholds.

Contribution

It presents a novel, continuous SFR model based on turbulence and density-dependent dynamical times, improving upon previous theories by removing ad-hoc density thresholds.

Findings

The model agrees with observed SFRs in molecular clouds.

It predicts two regimes with different SFR-density slopes.

A simplified formula for quick SFR estimates is provided.

Abstract

We present an analytical determination of the star formation rate (SFR) in molecular clouds, based on a time-dependent extension of our analytical theory of the stellar initial mass function (IMF). The theory yields SFR's in good agreement with observations, suggesting that turbulence {\it is} the dominant, initial process responsible for star formation. In contrast to previous SFR theories, the present one does not invoke an ad-hoc density threshold for star formation; instead, the SFR {\it continuously} increases with gas density, naturally yielding two different characteristic regimes, thus two different slopes in the SFR vs gas density relationship, in agreement with observational determinations. Besides the complete SFR derivation, we also provide a simplified expression, which reproduces reasonably well the complete calculations and can easily be used for quick determinations of SFR's in cloud environments. A key property at the heart of both our complete and simplified theory is that the SFR involves a {\it density-dependent dynamical time}, characteristic of each collapsing (prestellar) overdense region in the cloud, instead of one single mean or critical freefall timescale. Unfortunately, the SFR also depends on some ill determined parameters, such as the core-to-star mass conversion efficiency and the crossing timescale. Although we provide estimates for these parameters, their uncertainty hampers a precise quantitative determination of the SFR, within less than a factor of a few.