From the Core Mass Function to the Stellar Mass Function: The Efficiency Implied by Matching Their Peaks

This paper addresses a single question: If prestellar cores map onto stars one-to-one, what conversion efficiency is required to shift the observed core mass function peak onto the observed stellar mass function peak, and is that efficiency consistent with the outflow losses computed independently? Using published molecular-cloud and young-stellar-object measurements as inputs, and carrying the spin-torsion density bound of 9.72 x 10^57 kilograms per cubic metre and its critical shear of 8.56 x 10^32 per second as fixed comparison scales, the calculation finds that matching the peaks requires a core-to-star efficiency near 0.3, with a plausible range of about 0.25 to 0.35 across published core samples; that figure agrees with the fraction of a core that outflows can plausibly expel, giving two independent routes to the same loss factor, while competitive fragmentation of a thousand-solar-mass clump into roughly a thousand Jeans masses overproduces low-mass objects unless most fragments fail to collapse or later merge in the accounting. The headline values are: efficiency typical = 0.30; efficiency range = 0.29 to 0.33; N jeans = 1000.0. All values are computed from the stated formulae and inputs; this is a simulated and computed study, not a measurement. Where the comparison scales supplied by the torsion framework turn out to be too remote to influence the process, that outcome is reported as a negative result rather than passed over.