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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

It is well established that supermassive black hole (SMBH) feedback iscrucial for regulating the evolution of massive, if not all, galaxies. However,modelling the interplay between SMBHs and their host galaxies is challengingdue to the vast dynamic range. Previous simulations have utilized simplesubgrid models for SMBH accretion, while recent advancements track theproperties of the unresolved accretion disc, usually based on the thin$\alpha$-disc model. However, this neglects accretion in the radiativelyinefficient regime, expected to occur through a thick disc for a significantportion of an SMBH's lifetime. To address this, we present a novel 'unified'accretion disc model for SMBHs, harnessing results from the analyticaladvection-dominated inflow-outflow solution (ADIOS) model and state-of-the-artGR(R)MHD simulations. Going from low to high Eddington ratios, our modeltransitions from an ADIOS flow to a thin $\alpha$-disc via a truncated disc,incorporating self-consistently SMBH spin evolution due to Lense-Thirringprecession. Utilizing the moving mesh code AREPO, we perform simulations ofsingle and binary SMBHs within gaseous discs to validate our model and assessits impact. The disc state significantly affects observable luminosities, andwe predict markedly different electromagnetic counterparts in SMBH binaries.Crucially, the assumed disc model shapes SMBH spin magnitudes and orientations,parameters that gravitational wave observatories like LISA and IPTA are poisedto constrain. Our simulations emphasize the importance of accurately modellingSMBH accretion discs and spin evolution, as they modulate the availableaccretion power, profoundly shaping the interaction between SMBHs and theirhost galaxies.

A unified accretion disc model for supermassive black holes in galaxy formation simulations: method and implementation