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Cross-correlation-aided transport in stochastically driven accretion flows.

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This study explains linear instability in rotating accretion flows by showing how noise correlations interact with flow profiles. These interactions boost energy rates and influence wave dynamics, clarifying turbulence transition.

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Area of Science:

  • Plasma Physics
  • Astrophysics
  • Fluid Dynamics

Background:

  • The origin of linear instability in rotating sheared accretion flows, particularly in non-magnetized systems, has been a long-standing puzzle.
  • Previous research identified stochastic noise interacting with Taylor-Couette flow profiles as a source of instability, but excluded cross-correlations.

Purpose of the Study:

  • To investigate the impact of nonzero noise cross-correlations on linear instability in rotating accretion flows.
  • To resolve the dichotomy between magnetized and non-magnetized accretion flow instabilities by including noise cross-correlations.

Main Methods:

  • Introduction of time symmetry violating effects via nonzero noise cross-correlations.
  • Analysis of the renormalization of temporal correlations and its impact on energy rates and growth rates.
  • Examination of the influence on Alfven waves and autocorrelation functions.

Main Results:

  • Nonzero noise cross-correlations renormalize temporal correlations, boosting energy rates for spatial and temporal correlations.
  • Mutual competition in growth rates leads to suppression of oscillating Alfven waves at small times and faster saturation.
  • Noise cross-correlations magnify magnetic field strength and remove energy degeneracy in autocorrelation functions, leading to faster saturation with fewer oscillations.

Conclusions:

  • The findings convincingly explain subcritical transition to turbulence in the linear limit for all accretion flow scenarios.
  • This work establishes a benchmark for nonlinear stability studies in Keplerian accretion disks.