The Evolution of Pop III.1 Protostars Powered by Dark Matter Annihilation. I. Fiducial model and first results

TL;DR

This paper models the evolution of Population III.1 protostars influenced by dark matter annihilation, revealing conditions under which they can grow into supermassive stars and potentially seed early black holes, with implications for JWST observations.

Contribution

It introduces a comprehensive set of stellar evolution models for Pop III.1 stars considering dark matter effects, exploring parameter space to identify conditions for supermassive star formation.

Findings

Supermassive stars (>10^5 M_sun) require dark matter density >5×10^14 GeV/cm^3.

Dark matter annihilation inflates protostars, delaying hydrogen fusion onset.

Stars in dense halos (>10^15 GeV/cm^3) remain stable beyond 10^6 M_sun, affecting black hole seed formation.

Abstract

The existence of billion-solar-mass quasars at redshifts $z \gtrsim 7$ poses a formidable challenge to theories of black hole formation, requiring pathways for the rapid growth of massive seeds. Population III.1 stars, forming in pristine, dense dark matter (DM) minihalos, are compelling progenitors. This study presents a suite of stellar evolution models for accreting Pop III.1 protostars, calculated with the \textsc{GENEC} code. We systematically explore a wide parameter space, spanning ambient WIMP densities of $\rho_\chi \sim 10^{12}\mbox{-}10^{16}\,\mathrm{GeV\,cm^{-3}}$ and gas accretion rates of $10^{-3}\mbox{-}10^{-1}\,M_\odot\,\mathrm{yr^{-1}}$, to quantify the effects of DM annihilation. A central finding is that for a protostar to grow to supermassive scales ($\gtrsim 10^5 \, M_{\odot}$), the ambient DM density in the immediate vicinity of the star must exceed a critical threshold of $\rho_{\chi} \gtrsim 5 \times 10^{14} \, \text{GeV cm}^{-3}$. The energy injected by WIMP annihilation inflates the protostar, lowering its surface temperature, which suppresses the ionizing feedback that would otherwise halt accretion and significantly delays the onset of hydrogen fusion. This heating also governs the star's final fate: in dense halos ($\rho_\chi \gtrsim 10^{15}\,\mathrm{GeV\,cm^{-3}}$), stars remain stable against general relativistic instability beyond $10^6 \, M_{\odot}$, whereas at lower densities ($\rho_\chi \lesssim 10^{13}\,\mathrm{GeV\,cm^{-3}}$), they collapse at masses of $\sim 5 \times 10^5 \, M_{\odot}$. Once the DM fuel is exhausted and core burning commences, the protostar contracts and its ionising photon output can reach very high levels $\sim 10^{53} s^{-1}$. These distinct evolutionary phases offer clear observational signatures for the JWST, providing a robust, physically-grounded pathway for forming heavy black hole seeds in the early universe.