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

Evidence for dust around supermassive black holes (SMBHs) in the earlyUniverse is strongly suggested by recent observations. However, the accretionmechanism of SMBHs in dusty gas is not well understood yet. We investigate thegrowth of intermediate-mass black-holes (IMBHs) of $\sim 10^{5}~M_{\odot}$ industy clouds by using one-dimensional radiative-hydrodynamics simulations. Wefind that the accretion of dusty gas onto IMBHs proceeds gently with smallfluctuations of the accretion rate, whereas that of pristine gas causes moreviolent periodic bursts. At dust-to-gas mass ratios similar to the solarneighborhood, the time averaged luminosity becomes smaller than that forprimordial gas by one order of magnitude and the time-averaged Eddington ratioranges from $\sim 10^{-4}$ to $\sim 10^{-2}$ in clouds with initial gasdensities of $n_{\rm H} = 10 - 1000~\rm cm^{-3}$. Our calculations show thatthe effect of dust opacity alone is secondary compared to the radiationpressure on dust in regulating the BH growth. We also derive spectral energydistributions at IR bands by calculating dust thermal emission and show thatthe flux ratio between $\lambda \lesssim 20~\rm \mu m$ and $\gtrsim 100~\rm \mum$ is closely related to the Eddington ratio. Thermal emission from hot dustnear the BH dominates only during the high accretion phase, producing higherflux density at $\lesssim 20~\rm \mu m$. Therefore, we suggest that thecombinations of MIR observations by JWST and FIR observation by ALMA or Spitzercan be used to estimate the Eddington ratio of massive BHs.

Dusty Gas Accretion onto Massive Black Holes and Infrared Diagnosis of the Eddington Ratio