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

Article

Dobbie, Peter B., Kuncic, Zdenka, Bicknell, Geoffrey V. and Salmeron, Raquel. 2009. "Enhanced MHD Transport in Astrophysical Accretion Flows: Turbulence, Winds and Jets." Plasma and Fusion Research. 4, pp. 1-7. https://doi.org/10.1585/pfr.4.017

Article Title	Enhanced MHD Transport in Astrophysical Accretion Flows: Turbulence, Winds and Jets
ERA Journal ID	41197
Article Category	Article
Authors	Dobbie, Peter B. (Author), Kuncic, Zdenka (Author), Bicknell, Geoffrey V. (Author) and Salmeron, Raquel (Author)
Journal Title	Plasma and Fusion Research
Journal Citation	4, pp. 1-7
Number of Pages	7
Year	2009
Place of Publication	Japan
ISSN	1880-6821
Digital Object Identifier (DOI)	https://doi.org/10.1585/pfr.4.017
Web Address (URL)	https://www.jstage.jst.go.jp/article/pfr/4/0/4_0_017/_article
Abstract	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.
Keywords	MHD transport; Astrophysical accretion; astrophysical accretion disk; active galactic nucleus; X-ray binary; MHD (magnetohydrodynamics); numerical simulation
ANZSRC Field of Research 2020	510109. Stellar astronomy and planetary systems
Public Notes	Files associated with this item cannot be displayed due to copyright restrictions.
Byline Affiliations	University of Sydney
	Australian National University
Institution of Origin	University of Southern Queensland

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