Protostellar Outflow Energy Against Core Binding Energy: When a Single Outflow Can Unbind Its Parent Core

This paper addresses a single question: How does the mechanical energy carried by a protostellar outflow compare with the gravitational binding energy of the core that launched it, and what coupling efficiency would be required for outflows to disperse cores rather than merely stir them? 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 integrated outflow energies are comparable to, and for a low-mass core larger than, the core binding energy, so a coupling efficiency of tens of percent suffices in principle to disperse a low-mass core; for a cluster-forming clump the same comparison falls short by a factor of several, and outflow dispersal alone cannot unbind it. The headline values are: ratio lowmass = 5.20; ratio clump = 0.19; Ebind lowmass J = 5.77e+35. 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.