GW190521 formation scenarios via relativistic accretion

TL;DR

This paper explores how the GW190521 black hole merger could have originated from lower-mass progenitors that grew via relativistic accretion, considering different initial conditions and cosmic environments.

Contribution

It introduces a relativistic accretion model to trace the formation of GW190521 progenitors from lower initial masses at various redshifts, identifying three possible progenitor types.

Findings

Progenitors could be primordial, stellar-mass, or high-mass Pop III black holes.

Mass growth is sensitive to environmental density gradients and Mach number.

Variation in initial redshift has minimal impact on final masses.

Abstract

The recent gravitational wave transient GW190521 has been interpreted by the LIGO-Virgo collaboration (LVC) as sourced by a binary black hole (BH) merger. According to the LVC parameter estimation, at least one of these progenitors falls into the so-called pair-instability supernova mass gap. This raises the important question of how and when these progenitors formed. In this paper we use an accretion model with super-Eddington mass accretion rate obtained from General Relativity hydrodynamics simulations to analyse the scenario wherein the GW190521 original progenitors (OPs) formed at lower masses (and spins) and grew to their estimated LVC parameters by relativistic accretion. We consider that the environment wherein the binary is immersed has density gradients as well as a dependence on the Mach number of the gas. Taking the LVC parameter estimation at $z=0.82$ as the endpoint of the accretion evolution, we estimate the initial masses and spins of the OPs at three different red-shifts $z=100, \ 50$, and $20$. We found three distinct possible types of OPs: $(i)$ $10^{-4} M_{\odot} - 3 M_{\odot}$ almost non-rotating (with Kerr spin parameter $a_{\star}< 10^{-2}$) primordial BHs; $(ii)$ $3 M_{\odot} - 40M_{\odot}$ slowly rotating ($ 10^{-2} < a_{\star} < 0.5$) stellar mass BHs; $(iii)$ $40M_{\odot} - 70M_{\odot}$ BHs with a moderate spin parameter $a_{\star}\sim 0.5$, which could originate from the collapse of high mass Pop III stars. The mass spread is due to varying the density gradient and the relativistic Mach number of the cosmic plasma; the variation of the masses due to the origin at different red-shifts, on the other hand, is negligible, $\sim 2\%$ ...