Enhanced MHD Transport in Astrophysical Accretion Flows: Turbulence, Winds and Jets

Dobbie, Peter B. and Kuncic, Zdenka and Bicknell, Geoffrey V. and Salmeron, Raquel (2009) Enhanced MHD Transport in Astrophysical Accretion Flows: Turbulence, Winds and Jets. Plasma and Fusion Research: Review Articles, 4. pp. 1-7.


Astrophysical accretion is arguably the most prevalent physical process in the Universe; it occurs during the birth and death of individual stars and plays a pivotal role in the evolution of entire galaxies. Accretion onto a black hole, in particular, is also the most efficient mechanism known in nature, converting up to 40% of accreting rest mass energy into spectacular forms such as high-energy (X-ray and gamma-ray) emission and relativistic jets. Whilst magnetic fields are thought to be ultimately responsible for these phenomena, our understanding of the microphysics of MHD turbulence in accretion flows as well as large-scale MHD outflows remains far from complete. We present a new theoretical model for astrophysical disk accretion which considers enhanced vertical transport of momentum and energy by MHD winds and jets, as well as transport resulting from MHD turbulence. We also describe new global, 3D simulations that we are currently developing to investigate the extent to which non-ideal MHD effects may explain how small-scale, turbulent fields (generated by the magnetorotational instability — MRI) might evolve into large-scale, ordered fields that produce a magnetized corona and/or jets where the highest energy phenomena necessarily originate.

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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Files associated with this item cannot be displayed due to copyright restrictions.
Faculty/School / Institute/Centre: No Faculty
Faculty/School / Institute/Centre: No Faculty
Date Deposited: 21 Apr 2022 23:53
Last Modified: 21 Apr 2022 23:53
Uncontrolled Keywords: MHD transport; Astrophysical accretion; astrophysical accretion disk; active galactic nucleus; X-ray binary; MHD (magnetohydrodynamics); numerical simulation
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Socio-Economic Objectives (2020): 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences
Identification Number or DOI: https://doi.org/10.1585/pfr.4.017
URI: http://eprints.usq.edu.au/id/eprint/47848

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