Filling the Black Hole Mass Gap: Avoiding Pair Instability in Massive Stars through Addition of Non-Nuclear Energy

Abstract

In standard stellar evolution, stars with masses ranging from approximately $150$ to $240M_{\odot }$ are expected to evolve to a pair instability supernova with no black hole (BH) remnant. This evolutionary behavior leads to a predicted gap in the black hole mass function from approximately $50$ to $140M_{\odot }$. Yet the LIGO and Virgo Collaborations[1] recently discovered black holes of masses $66M_{\odot }$ and $85M_{\odot }$ in the gravitational wave event GW190521. We propose a new method to populate the BH mass gap. If an energy source is added throughout the star in addition to nuclear fusion, it is possible for the altered evolution to avoid the complete destruction of a pair instability supernova, and instead a BH remnant is left behind. An example of an extra energy source is dark matter annihilation within the star, but our results hold more generally. We show this phenomenon by exploring the effect of adding an energy source independent of temperature and density to a $180M_{\odot }$ star, using the MESA one-dimensional stellar evolution software. If $\sim 50$\% of the star's energy is due to this new source, the star is capable of avoiding the pair instability entirely and evolving towards a core-collapse supernova and ultimately a BH remnant with mass $\sim 120M_{\odot }$.

20 pages, 9 figures, 2 tables

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