English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Large dynamic range numerical simulations of atomic cooling driven collapse of gas in pre‐galactic dark matter haloes with   T  vir ∼ 10 000  K  show that the gas loses 90  per cent and more of its angular momentum before rotational support sets in. In a fraction of these haloes where the metallicity is low and ultraviolet (UV) radiation suppresses  H  2  cooling, conditions are thus very favourable for the rapid build‐up of massive black holes. Depending on the progression of metal enrichment, the continued suppression of  H  2  cooling by external and internal UV radiation and the ability to trap the entropy produced by the release of gravitational energy, the gas at the centre of the halo is expected to form a supermassive star, a stellar‐mass black hole accreting at super‐Eddington accretion rates or a compact star‐cluster undergoing collisional run‐away of massive stars at its centre. In all three cases, a massive black hole of initially modest mass finds itself at the centre of a rapid inflow of gas with inflow rates of  ≳1 M ⊙  yr −1  . The massive black hole will thus grow quickly to a mass of  10 5 – 10 6  M ⊙   until further inflow is halted either by consumption of gas by star formation or by the increasing energy and momentum feedback from the growing massive black hole. Conditions for the formation of massive seed black holes in this way are most favourable in haloes with   T  vir ∼ 15 000 K  and   V  vir ∼ 20  km  s −1   with less massive haloes not allowing collapse of gas by atomic cooling and more massive haloes being more prone to fragmentation. This should imprint a characteristic mass on the mass spectrum of an early population of massive black hole seeds in pre‐galactic haloes which will later grow into the observed population of supermassive black holes in galactic bulges.

Pathways to massive black holes and compact star clusters in pre‐galactic dark matter haloes with virial temperatures ≳10 000 K