Evolution and explosions of metal enriched supermassive stars: proton rich general relativistic instability supernovae

TL;DR

This paper investigates the collapse and potential explosion of metal-enriched supermassive stars due to general relativistic instability, exploring their nucleosynthesis and implications for early universe black hole formation.

Contribution

It provides the first detailed simulations of metal-rich supermassive star collapse, including hydrodynamics and nucleosynthesis, revealing explosion conditions and elemental yields.

Findings

Supermassive stars can explode due to relativistic instability with specific metallicities.

Explosions produce enhanced nitrogen and intermediate mass elements.

Results suggest a link to observed super-solar nitrogen in high-redshift galaxies.

Abstract

The assembly of supermassive black holes poses a challenge primarily because of observed quasars at high redshift, but additionally because of the current lack of observations of intermediate mass black holes. One plausible scenario for creating supermassive black holes is direct collapse triggered by the merger of two gas rich galaxies. This scenario allows the creation of supermassive stars with solar metallicity, where the enhanced metallicity is enabled by extremely rapid accretion. We investigate the behavior of metal enriched supermassive stars which collapse due to the general relativistic radial instability during hydrogen burning. These stars contain both hydrogen and metals and thus may explode due to the CNO cycle (carbon-nitrogen-oxygen) and the rp process (rapid proton capture). We perform a suite of stellar evolution simulations for a range of masses and metallicities, both including and neglecting mass loss. We evaluate the stability of these supermassive stars by solving the pulsation equation in general relativity. When the stars becomes unstable, we perform 1D general relativistic hydrodynamical simulations coupled to a 153 isotope nuclear network with cooling from neutrino reactions, in order to determine if the stars explode. If the stars do explode, we post process the nucleosynthesis using a 514 isotope network which includes additional proton rich isotopes. These explosions are characterized by enhanced nitrogen and intermediate mass elements ($16\geq\rm{A}\geq25$), and suppressed light elements ($8\geq\rm{A}\geq14$), and we comment on recent observations of super-solar nitrogen in GN-z11.