Rapidly accreting supermassive stars: reliable determination of the final mass

Abstract

Supermassive black holes might form by direct collapse, with a supermassive star (SMS) as progenitor. In this scenario, the SMS accretes at > 0.1 Msun/yr until it collapses into a massive black hole seed due to the general-relativistic (GR) instability. However, the exact mass at which the collapse occurs is not known, as existing numerical simulations give divergent results. Here, this problem is addressed analytically, which allows for ab initio, reliable determination of the onset point of the GR instability, for given hydrostatic structures. We apply the relativistic equation of radial pulsations in its general form to the hydrostatic GENEC models already published. We show that the mass of spherical SMSs forming in atomically cooled haloes cannot exceed 500 000 Msun, in contrast to previous claims. On the other hand, masses in excess of this limit, up to 10^6 Msun, could be reached in alternative versions of direct collapse. Our method can be used to test the consistency of GR hydrodynamical stellar evolution codes.

References in corpus (4)

• The Evolution of Supermassive Population III Stars
• The Final Fates of Accreting Supermassive Stars
• Formation of primordial supermassive stars by burst accretion
• Maximally accreting supermassive stars: a fundamental limit imposed by hydrostatic equilibrium

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• Ionizing photon production of Population III stars: effects of rotation, convection, and initial mass function
• Evolution and explosions of metal enriched supermassive stars: proton rich general relativistic instability supernovae
• Pulsations of primordial supermassive stars induced by a general relativistic instability; visible to JWST at z$>$12
• The Evolution of Accreting Population III Stars at 10${}^{-6}$-10${}^3$ M${}_{\odot }$/yr
• Linear adiabatic analysis for general relativistic instability in primordial accreting supermassive stars
• General-relativistic instability in rapidly accreting supermassive stars in the presence of dark matter
• Probing supermassive stars and massive black hole seeds through gravitational wave inspirals
• The properties of supermassive stars in galaxy merger driven direct collapse I: models without rotation