Astrophysical Black holes: An Explanation for the Galaxy Quenching

TL;DR

This paper explores models of astrophysical black holes without event horizons as a potential explanation for galaxy quenching, contrasting them with traditional black holes and analyzing their observational signatures.

Contribution

It introduces models of ABHs without event horizons and compares their feedback mechanisms and observational features to those of classical black holes.

Findings

ABHs without event horizons can generate stronger winds from accretion disks.

Differences in feedback mechanisms between BHs and ABHs are identified.

Potential observational signatures of stellar-mass ABHs are proposed.

Abstract

In light of increasing observational evidence supporting the existence of ultra-compact objects, we adopt the term astrophysical black hole to refer to any object having a huge mass confined within a sufficiently small region of spacetime. This terminology encompasses both the classical black hole solutions predicted by general relativity, as well as alternative compact objects that may not possess an event horizon. We propose models of Astrophysical Black holes (ABHs) without event horizons (EHs), as a more viable explanation for the long-term quenching phenomenon in galaxies. At the same time, the short-term quenching is explained here in terms of an efficient feedback expected in the models of stellar-mass astrophysical black holes (StMABHs). We have calculated the radiative flux from the disk in a general spherically symmetric metric background and used it to contrast the distinctive features of the BHs and ABHs scenarios. We demonstrate the relative ease of wind generation from the accretion disk surrounding an ABH without an event horizon, compared to a BH, and highlight the significant strength of these winds. The nature of the feedbacks arising from accretion onto a BH and an ABH in the `quasar' and `radio' modes are compared and some possible observational signatures of the StMABHs are pointed out.