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The Quasi-star Channel of Supermassive Black Hole Formation

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If you have a question about this talk, please contact Sandro Tacchella .

An increasing body of evidence indicates that the seeds of supermassive black holes had to form very early and grow very rapidly. An intriguing mechanism for accomplishing this is via the core collapse of supermassive stars, which leaves behind an intermediate-mass black hole embedded in a much more massive envelope from which it accretes at a hyper-Eddington rate. The properties of such hypothetical objects, called quasi-stars, are well-constrained theoretically. In their latter stages of evolution, they are predicted to resemble the “Little Red Dots” discovered by JWST . If LRDs are indeed late-stage quasi-stars, their short predicted lifetimes suggest that the quasi-star channel is an important mode of supermassive black hole formation and early growth.

This talk is part of the Galaxies Discussion Group series.

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