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

There is compelling evidence that most -if not all- galaxies harbour asuper-massive black hole (SMBH) at their nucleus, hence binaries of thesemassive objects are an inevitable product of the hierarchical evolution ofstructures in the universe, and represent an important but thus-far elusivephase of galaxy evolution. Gas accretion via a circumbinary disc is thought tobe important for the dynamical evolution of SMBH binaries, as well as inproducing luminous emission that can be used to infer their properties. Oneplausible source of the gaseous fuel is clumps of gas formed due to turbulenceand gravitational instabilities in the interstellar medium, that later falltoward and interact with the binary. In this context, we model numerically theevolution of turbulent clouds in near-radial infall onto equal-mass SMBHbinaries, using a modified version of the SPH code GADGET-3. We present a totalof 12 simulations that explore different possible pericentre distances andrelative inclinations, and show that the formation of circumbinary discs anddiscs around each SMBH ('mini-discs') depend on those parameters. We also studythe dynamics of the formed discs, and the variability of the feeding rate ontothe SMBHs in the different configurations.

Infalling clouds onto super-massive black hole binaries - I. Formation of discs, accretion and gas dynamics