Chaos in Turbulence Driven by the Magnetorotational Instability

Details Chaos in Turbulence Driven by the Magnetorotational Instability Chaos in Turbulence Driven by the Magnetorotational Instability

2003-01-24

arxiv.org/abs/astro-ph/0301498v1

Astronomy and Astrophysics

Astrophysics

6 pages, 8 figures. To be appear in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06315.x

Chaotic flow is studied in a series of numerical magnetohydrodynamical simulations that use the shearing box formalism. This mimics important features of local accretion disk dynamics. The magnetorotational instability gives rise to flow turbulence, and quantitative chaos parameters, such as the largest Lyapunov exponent, can be measured. Linear growth rates appear in these exponents even when the flow is fully turbulent. The extreme sensitivity to initial conditions associated with chaotic flows has practical implications, the most important of which is that hundreds of orbital times are needed to extract a meaningful average for the stress. If the evolution time in a disk is less than this, the classical $\alpha$ formalism will break down.

Affiliated with

Also associated with

No associations

Rating

Chaos in Turbulence Driven by the Magnetorotational Instability does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Chaos in Turbulence Driven by the Magnetorotational Instability, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Chaos in Turbulence Driven by the Magnetorotational Instability will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-709445