The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs

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The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs. / Pessah, Martin Elias; Chan, Chi-kwan; Psaltis, Dimitrios.

I: Monthly Notices of the Royal Astronomical Society, Bind 372, Nr. 1, 24.08.2006, s. 183-190.

Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt

Harvard

Pessah, ME, Chan, C & Psaltis, D 2006, 'The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs', Monthly Notices of the Royal Astronomical Society, bind 372, nr. 1, s. 183-190. https://doi.org/10.1111/j.1365-2966.2006.10824.x

APA

Pessah, M. E., Chan, C., & Psaltis, D. (2006). The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs. Monthly Notices of the Royal Astronomical Society, 372(1), 183-190. https://doi.org/10.1111/j.1365-2966.2006.10824.x

Vancouver

Pessah ME, Chan C, Psaltis D. The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs. Monthly Notices of the Royal Astronomical Society. 2006 aug. 24;372(1):183-190. https://doi.org/10.1111/j.1365-2966.2006.10824.x

Author

Pessah, Martin Elias ; Chan, Chi-kwan ; Psaltis, Dimitrios. / The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs. I: Monthly Notices of the Royal Astronomical Society. 2006 ; Bind 372, Nr. 1. s. 183-190.

Bibtex

@article{9f33e2c120034c60a6efe0d403a5adbf,
title = "The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs",
abstract = "The magnetorotational instability is thought to be responsible for the generation of magnetohydrodynamic turbulence that leads to enhanced outward angular momentum transport in accretion discs. Here, we present the first formal analytical proof showing that, during the exponential growth of the instability, the mean (averaged over the disc scale-height) Reynolds stress is always positive, the mean Maxwell stress is always negative, and hence the mean total stress is positive and leads to a net outward flux of angular momentum. More importantly, we show that the ratio of the Maxwell to the Reynolds stresses during the late times of the exponential growth of the instability is determined only by the local shear and does not depend on the initial spectrum of perturbations or the strength of the seed magnetic. Even though we derived these properties of the stress tensors for the exponential growth of the instability in incompressible flows, numerical simulations of shearing boxes show that this characteristic is qualitatively preserved under more general conditions, even during the saturated turbulent state generated by the instability.",
keywords = "astro-ph",
author = "Pessah, {Martin Elias} and Chi-kwan Chan and Dimitrios Psaltis",
year = "2006",
month = aug,
day = "24",
doi = "10.1111/j.1365-2966.2006.10824.x",
language = "English",
volume = "372",
pages = "183--190",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

RIS

TY - JOUR

T1 - The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs

AU - Pessah, Martin Elias

AU - Chan, Chi-kwan

AU - Psaltis, Dimitrios

PY - 2006/8/24

Y1 - 2006/8/24

N2 - The magnetorotational instability is thought to be responsible for the generation of magnetohydrodynamic turbulence that leads to enhanced outward angular momentum transport in accretion discs. Here, we present the first formal analytical proof showing that, during the exponential growth of the instability, the mean (averaged over the disc scale-height) Reynolds stress is always positive, the mean Maxwell stress is always negative, and hence the mean total stress is positive and leads to a net outward flux of angular momentum. More importantly, we show that the ratio of the Maxwell to the Reynolds stresses during the late times of the exponential growth of the instability is determined only by the local shear and does not depend on the initial spectrum of perturbations or the strength of the seed magnetic. Even though we derived these properties of the stress tensors for the exponential growth of the instability in incompressible flows, numerical simulations of shearing boxes show that this characteristic is qualitatively preserved under more general conditions, even during the saturated turbulent state generated by the instability.

AB - The magnetorotational instability is thought to be responsible for the generation of magnetohydrodynamic turbulence that leads to enhanced outward angular momentum transport in accretion discs. Here, we present the first formal analytical proof showing that, during the exponential growth of the instability, the mean (averaged over the disc scale-height) Reynolds stress is always positive, the mean Maxwell stress is always negative, and hence the mean total stress is positive and leads to a net outward flux of angular momentum. More importantly, we show that the ratio of the Maxwell to the Reynolds stresses during the late times of the exponential growth of the instability is determined only by the local shear and does not depend on the initial spectrum of perturbations or the strength of the seed magnetic. Even though we derived these properties of the stress tensors for the exponential growth of the instability in incompressible flows, numerical simulations of shearing boxes show that this characteristic is qualitatively preserved under more general conditions, even during the saturated turbulent state generated by the instability.

KW - astro-ph

U2 - 10.1111/j.1365-2966.2006.10824.x

DO - 10.1111/j.1365-2966.2006.10824.x

M3 - Journal article

VL - 372

SP - 183

EP - 190

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 1

ER -

ID: 34382806