  Standard stellar evolution models predict that black holes in the range of
approximately $50 - 140 M_\odot$ should not exist directly from stellar
evolution. This gap appears because stars with masses between 100 and 240
$M_\odot$ are expected to undergo a pair instability supernova and leave behind
no remnant, or a pulsational pair instability supernova and leave behind a
remnant much smaller than their initial stellar mass. However, black holes have
been discovered by the LIGO/Virgo collaboration within this mass range. In
previous work (arXiv:2010.00254), we used the stellar evolution code MESA to
show that the addition of non-nuclear energy (such as from annihilation of dark
matter) could alter the evolution of a 180 $M_\odot$ star so that the observed
black holes could be produced from isolated stars. In this paper, we extend
this analysis to stars of other masses, and find that sufficient amounts of
non-nuclear energy can allow any star to avoid pair instability, and could
produce a black hole of mass comparable to the initial stellar mass. In
addition, we produce examples of the type of black hole initial mass function
that can be produced from this mechanism. These illustrative examples suggest
that adding non-nuclear energy to stars offers a way to fully close the mass
gap.

High Energy Astrophysical Phenomena;Cosmology and Nongalactic Astrophysics;Solar and Stellar Astrophysics