A One-Dimensional Model for Star Formation Near a "Leaky" Black Hole

TL;DR

This paper proposes a one-dimensional model for star formation near a 'leaky' black hole, driven by black hole wind emissions, potentially explaining young stars observed close to Sagittarius A*.

Contribution

It introduces a novel model linking black hole wind emissions to star formation, incorporating disk stability analysis and angular momentum mechanisms.

Findings

Identifies conditions for disk collapse due to black hole wind.

Estimates collapse times for star-forming disks.

Suggests a mechanism for disk angular momentum acquisition.

Abstract

In the presence of a Weyl scaling invariant cosmological action, black holes no longer have an event horizon and an apparent horizon. So they have no trapped surfaces, and may be "leaky", emitting a "black hole wind" which could lead to star formation in the neighborhood of the hole. In this paper we formulate and analyze a one-dimensional model for star formation resulting from a postulated outgoing black hole particle flux, incident on a distant spherical surface modeled as a set of planar disks surrounding the hole. Using the Toomre analysis of the Jeans instability of a disk, we compute conditions for a disk collapse instability and estimate the collapse time. We suggest a mechanism for giving the disk angular momentum around the central black hole. This gives a possible explanation for the puzzling observation of young stars forming in the vicinity of the black hole Sagittarius A* central to the Milky Way galaxy.