Radiative feedback on supermassive star formation: the massive end of the Population III initial mass function

Abstract

Supermassive stars (SMSs) with masses of $M_{\ast }\simeq 10^4$--$10^5{\mathrm{M}}_{\odot }$ are invoked as possible seeds of high-redshift supermassive black holes, but it remains under debate whether their protostar indeed acquires sufficient mass via gas accretion overcoming radiative feedback. We investigate protostellar growth in dynamically heated atomic-cooling haloes (ACHs) found in recent cosmological simulations, performing three-dimensional radiation hydrodynamical (RHD) simulations that consider stellar evolution under variable mass accretion. We find that one of the ACHs feeds the central protostar at rates exceeding a critical value, above which the star evolves in a cool bloating phase and hardly produces ionizing photons. Consequently, the stellar mass reaches $M_{\ast }\gtrsim 10^4{\mathrm{M}}_{\odot }$ unimpeded by radiative feedback. In the other ACH, where the mass supply rate is lower, the star spends most of its life as a hot main-sequence star, emitting intense ionizing radiation. Then, the stellar mass growth is terminated around $500{\mathrm{M}}_{\odot }$ by photoevaporation of the circumstellar disk. A series of our RHD simulations provide a formula of the final stellar mass determined either by stellar feedback or their lifetime as a function of the mass supply rate from the parent cloud in the absence of stellar radiation. Combining the results with the statistical properties of SMS-forming clouds in high-redshift quasar progenitor haloes, we construct a top-heavy mass distribution of primordial stars over $M_{\ast }\simeq 100$--$10^5{\mathrm{M}}_{\odot }$, approximately following a power-law spectrum of $\propto M_{\ast }^{-1.3}$ with a steeper decline at $M_{\ast }\gtrsim 2\times 10^4{\mathrm{M}}_{\odot }$. Their massive BH remnants would be further fed via the dense debris disk, powering "milli-quasars" with a bolometric luminosity of $L_{\mathrm{bol}}\gtrsim 10^{43}\mathrm{erg}{\mathrm{s}}^{-1}$.

arXiv comment16 pages, 12 figures, and 3 tables, submitted to MNRAS

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