Growth of massive black holes at high-z via accretion predominantly driven by magnetic outflows

Abstract

Luminous quasars powered by accreting supermassive black holes (SMBHs) have been found in the early Universe at $z\gtrsim 7.5$, which set a strong constraint on both the seed black hole mass and the rapid growth of the SMBHs. In this work, we explore how the SMBHs are grown through Eddington limited accretion driven predominantly by magnetic outflows. Most angular momentum and the released gravitational energy in the disk can be removed by magnetic outflows, and therefore the mass accretion rate of the black hole (BH) can be high even if the disk is radiating at sub-Eddington luminosity. It is found that the SMBH with several billion solar masses discovered at $z\gtrsim 7$ may probably be grown through chaotic accretion predominantly driven by magnetic outflows from a stellar mass BH, when the disks are radiating at moderate luminosity ($\sim 0.5$ Eddington luminosity) with mild outflows. We find that most SMBHs are spinning at moderate values of spin parameter $a_{\ast }$, which implies only a small fraction of quasars may have radio jets.

14 pages, 7 figures, 1 table, accepted for publication in ApJ

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Cited by in corpus (6)

• Application of the disk instability model to all Quasi-Periodic Eruptions
• A magnetic accretion disk-outflow model for changing look active galactic nuclei
• The large-scale magnetic field advected in the corona of a thin accretion disk
• Hypercritical accretion during common envelopes in triples leading to binary black holes in the pair-instability-supernova mass gap
• Probing the Growth of Massive Black Holes with Black Hole-Host Galaxy Spin Correlations
• Direct Collapse to Precursors of Supermassive Black Hole Seeds:Radiation-feedback-generated Outflows