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Cited by 271Astrophysical Phenomena and ObservationsGalaxies: Formation, Evolution, PhenomenaAstrophysics and Star Formation Studies

NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. II. NATURE, ORIGIN, AND PROPERTIES OF OUTFLOWS AND THEIR POSSIBLE OBSERVATIONAL APPLICATIONS

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Yuan, Feng, Bu, Defu, Wu, Maochun·2012·The Astrophysical Journal
DOI 10.1088/0004-637x/761/2/130
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Abstract

Hydrodynamical (HD) and magnetohydrodynamical (MHD) numerical simulations of hot accretion flows have indicated that the inflow accretion rate decreases inward. Two models have been proposed to explain this result. In the adiabatic inflow–outflow solution (ADIOS), this is because of the loss of gas in the outflow. In the alternative convection-dominated accretion flow model, it is thought that the flow is convectively unstable and gas is locked in convective eddies. We investigate the nature of the inward decrease of the accretion rate using HD and MHD simulations. We calculate various properties of the inflow and outflow such as temperature and rotational velocity. Systematic and significant differences are found. These results suggest that the inflow and outflow are not simply convective turbulence; instead, systematic inward and outward motion (i.e., real outflow) must exist. We have also analyzed the convective stability of MHD accretion flows and found that they are stable. These results favor the ADIOS scenario. We suggest that the mechanisms of producing outflow in HD and MHD flows are the buoyancy associated with the convection and the centrifugal force associated with the angular momentum transport mediated by the magnetic field, respectively. The latter is similar to the Blandford & Payne mechanism but no large-scale open magnetic field is required. We discuss some possible observational applications, including the Fermi bubble in the Galactic center and winds in active galactic nuclei and black hole X-ray binaries.

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Crossref · 10.1088/0004-637x/761/2/130

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  • If the accretion rate is ≲10^-3 of the Eddington rate, the density in the accretion disk around the supermassive black hole is low enough to form a non-radiative accretion flow, which can lead to formation of collimated outflows such as jets.

    “If ˙ M acc / ˙ M edd ≲ 10 -3 , then the density in the accretion disk around the SMBH is low enough to form a non-radiative accretion flow which can lead to formation of collimated outflows such as jets (Narayan & Yi 1995; Yuan et al. 2012; Yuan & Narayan 2014; Giustini & Proga 2019).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Yuan et al. 2012

  • Wide-angle winds can also be generated due to magnetic field-mediated centrifugal force or simple buoyancy in the accretion disk in highly accreting systems.

    “Alternatively, wide-angle winds can also be generated due to magnetic field-mediated centrifugal force or simple buoyancy in the accretion disk in such highly accreting systems (Yuan et al. 2012; Jiang et al. 2014, 2019).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Yuan et al. 2012

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Authors
Yuan, F., Bu, D., & Wu, M.
Affiliations
  • Xiamen University (CN)
  • Chinese Academy of Sciences (CN)
Corresponding author
  • Yuan, Feng
  • Wu, Maochun
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2012-12-04
Volume
761
Issue
2
Pages
130
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/761/2/130
OpenAlex
W2167436765
Cited by
271
References
127
Citations by year
2026: 17 · 2025: 9 · 2024: 11 · 2023: 19 · 2022: 22 · 2021: 12 · 2020: 24 · 2019: 24 · 2018: 31 · 2017: 18 · 2016: 23 · 2015: 16 · 2014: 16 · 2013: 25 · 2012: 4
FWCI
10.68
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • arXiv (Cornell University)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Keywords
hot accretion flows, accretion outflows, convective instability, magnetohydrodynamic accretion, angular momentum transport, Fermi bubbles, black hole X-ray binaries

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