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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Accretion on to seed black holes (BHs) is believed to play a crucial role information of supermassive BHs observed at high-redshift (z>6). Here, weinvestigate the combined effect of gas angular momentum and radiation feedbackon the accretion flow, by performing 2D axially symmetric radiationhydrodynamics simulations that solve the flow structure across the Bondi radiusand the outer part of the accretion disc simultaneously. The accreting gas withfinite angular momentum forms a rotationally-supported disc inside the Bondiradius, where the accretion proceeds by the angular momentum transport due toassumed alpha-type viscosity. We find that the interplay of radiation andangular momentum significantly suppresses accretion even if the radiativefeedback is weakened in an equatorial shadowing region. The accretion rate isO(alpha)\sim O(0.01-0.1) times the Bondi value, where alpha is the viscosityparameter. By developing an analytical model, we show that such a greatreduction of the accretion rate persists unless the angular momentum is sosmall that the corresponding centrifugal radius is \lesssim 0.04 times theBondi radius. We argue that BHs are hard to grow quickly via rapid massaccretion considering the angular momentum barrier presented in this paper.

Stunted accretion growth of black holes by combined effect of the flow angular momentum and radiation feedback