A test of the conjectured critical black-hole formation -- null geodesic correspondence: The case of self-gravitating scalar fields

TL;DR

This paper tests a conjecture linking black-hole formation thresholds to null geodesic stability by analytically and numerically analyzing self-gravitating scalar fields near collapse, finding good agreement between theory and simulation.

Contribution

It provides the first non-trivial analytical test of the conjectured correspondence using self-gravitating scalar fields and compares results with detailed numerical simulations.

Findings

Analytical critical compactness parameter matches numerical value within 10%.

Null geodesic stability correlates with black-hole formation threshold.

Supports the conjectured link between geodesic properties and collapse dynamics.

Abstract

It has recently been conjectured [A. Ianniccari {\it et al.}, Phys. Rev. Lett. {\bf 133}, 081401 (2024)] that there exists a correspondence between the critical threshold of black-hole formation and the stability properties of null circular geodesics in the curved spacetime of the collapsing matter configuration. In the present compact paper we provide a non-trivial test of this intriguing conjecture. In particular, using analytical techniques we study the physical and mathematical properties of self-gravitating scalar field configurations that possess marginally-stable (degenerate) null circular geodesics. We reveal the interesting fact that the {\it analytically} calculated critical compactness parameter ${\cal C}^{\text{analytical}}\equiv{\text{max}_r}\{m(r)/r\}=6/25$, which signals the appearance of the first (marginally-stable) null circular geodesic in the curved spacetime of the self-gravitating scalar fields, agrees quite well (to within $\sim10\%$) with the exact compactness parameter ${\cal C}^{\text{numerical}}\equiv\text{max}_t\{\text{max}_r\{m(r)/r\}\}\simeq0.265$ which is computed {\it numerically} using fully non-linear numerical simulations of the gravitational collapse of scalar fields at the threshold of black-hole formation [here $m(r)$ is the gravitational mass contained within a sphere of radius $r$].