The fundamental difference between shear alpha viscosity and turbulent magnetorotational stresses

Martin E. Pessah, Chi Kwan Chan, Dimitrios Psaltis

Research output: Contribution to journalArticle

32 Citations (Scopus)

Abstract

Numerical simulations of turbulent, magnetized, differentially rotating flows driven by the magnetorotational instability (MRI) are often used to calculate the effective values of alpha viscosity that is invoked in analytical models of accretion discs. In this paper, we use various dynamical models of turbulent magnetohydrodynamic stresses, as well as numerical simulations of shearing boxes, to show that angular momentum transport in MRI-driven accretion discs cannot be described by the standard model for shear viscosity. In particular, we demonstrate that turbulent magnetorotational stresses are not linearly proportional to the local shear and vanish identically for angular velocity profiles that increase outwards.

Original languageEnglish (US)
Pages (from-to)683-690
Number of pages8
JournalMonthly Notices of the Royal Astronomical Society
Volume383
Issue number2
DOIs
StatePublished - Jan 2008

Fingerprint

accretion disks
viscosity
shear
angular velocity
shearing
accretion
rotating flow
magnetohydrodynamics
boxes
angular momentum
simulation
velocity distribution
velocity profile

Keywords

  • Accretion, accretion discs
  • Black hole physics
  • Instabilities
  • MHD
  • Turbulence

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

The fundamental difference between shear alpha viscosity and turbulent magnetorotational stresses. / Pessah, Martin E.; Chan, Chi Kwan; Psaltis, Dimitrios.

In: Monthly Notices of the Royal Astronomical Society, Vol. 383, No. 2, 01.2008, p. 683-690.

Research output: Contribution to journalArticle

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