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Direct collapse to SMBH seeds in cosmological halos with radiation transfer

Published online by Cambridge University Press:  10 June 2020

Kentaro Nagamine Open the ORCID record for Kentaro Nagamine [Opens in a new window] ,
Isaac Shlosman  and
Yang Luo
Kentaro Nagamine
Affiliation:
Theoretical Astrophysics, Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka560-0043, Japan email: [email protected] Department of Physics & Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy, Las Vegas, NV89154-4002, USA Kavli IPMU (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba, 277-8583, Japan
Isaac Shlosman
Affiliation:
Theoretical Astrophysics, Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka560-0043, Japan email: [email protected] Department of Physics & Astronomy, University of Kentucky, Lexington, KY40506-0055, USA
Yang Luo
Affiliation:
Department of Astronomy and Jiujiang Research Institute, Xiamen University, Xiamen, Fujian361005, People’s Republic of China
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Abstract

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We present results of our zoom-in cosmological hydrodynamic simulations of direct collapse (DC) to supermassive black hole (SMBH) seeds with radiative transfer (RT). The DC has been modeled in dark matter halos of ∼108M⊙, using adaptive mesh refinement (AMR) code Enzo. For the first time, the baryonic collapse has been followed down to 10−7 pc (∼0.01 AU) with on-the-fly RT and the flux-limited diffusion (FLD) approximation. We find a complex behavior involving accretion flow and associated outflows driven by the radiation force. The resulting gas dynamics around the central density peak differs profoundly from that in previous works which adopted adiabatic approximation in the core. The core forms with a photosphere at ∼1 AU, and its growth starts to saturate at ∼100M⊙. The unrelaxed core radiates intermittently near the Eddington luminosity, correlated with strong anisotropic outflows.

Keywords

hydrodynamicsblack hole physicsradiative transferaccretionmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 289 - 291
Copyright
© International Astronomical Union 2020

References

Ardaneh, K., Luo, Y., Shlosman, I., Nagamine, K., et al. 2018, MNRAS, 479, 227710.1093/mnras/sty1657CrossRefGoogle Scholar
Hahn, O. & Abel, T. 2011, MNRAS, 415, 210110.1111/j.1365-2966.2011.18820.xCrossRefGoogle Scholar
Mayer, M. & Duschl, W. J. 2005, MNRAS, 358, 61410.1111/j.1365-2966.2005.08826.xCrossRefGoogle Scholar
Luo, Y., Nagamine, K., & Shlosman, I. 2016, MNRAS, 459, 321710.1093/mnras/stw698CrossRefGoogle Scholar
Luo, Y., Ardaneh, K., Shlosman, I., Nagamine, K., et al. 2018, MNRAS, 476, 352310.1093/mnras/sty362CrossRefGoogle Scholar
Reynolds, D. R., et al. 2009, Journal of Computational Physics, 228, 683310.1016/j.jcp.2009.06.006CrossRefGoogle Scholar
Shlosman, I., Choi, J.-H., Begelman, M. C., & Nagamine, K. 2016, MNRAS, 456, 50010.1093/mnras/stv2700CrossRefGoogle Scholar