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Turbulent Flow01:24

Turbulent Flow

146
Turbulent flow is characterized by unpredictable fluctuations in velocity and pressure, which result in a chaotic fluid movement distinct from the orderly patterns of laminar flow. While laminar flow is governed by smooth, parallel layers with minimal mixing, turbulent flow exhibits highly irregular, three-dimensional patterns. This behavior arises due to instabilities in the fluid's velocity profile, and amplifies as the flow velocity increases. Minor disturbances, known as turbulent...
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Laminar and Turbulent Flow01:07

Laminar and Turbulent Flow

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Fluid dynamics is the study of fluids in motion. Velocity vectors are often used to illustrate fluid motion in applications like meteorology. For example, wind—the fluid motion of air in the atmosphere—can be represented by vectors indicating the speed and direction of the wind at any given point on a map. Another method for representing fluid motion is a streamline. A streamline represents the path of a small volume of fluid as it flows. When the flow pattern changes with time, the...
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Boundary Layer Characteristics01:18

Boundary Layer Characteristics

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When a fluid encounters a solid surface, a boundary layer forms due to the interaction between the fluid's motion and the stationary surface. This phenomenon is characterized by a thin region adjacent to the surface where viscous forces dominate, influencing the fluid's velocity profile. The development of the boundary layer begins at the leading edge of the surface and evolves as the fluid moves downstream.As the fluid flows over the surface, friction between the fluid and the wall slows down...
57
Poiseuille's Law and Reynolds Number01:10

Poiseuille's Law and Reynolds Number

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Any fluid in a horizontal tube can flow due to pressure differences—fluid flows from high to low pressure. The flow rate (Q) is the ratio of pressure difference and resistance through a horizontal tube. The greater the pressure difference, the higher the flow rate. The flow resistance is expressed as:
6.4K
Navier–Stokes Equations01:28

Navier–Stokes Equations

430
For incompressible Newtonian fluids, where density remains constant, stresses show a linear relationship with the deformation rate, defined by normal and shear stresses. Normal stresses depend on the pressure exerted on the fluid and the rate of deformation in specific directions, which determines how fluid flows under varying pressures. Shear stresses, on the other hand, act tangentially across fluid layers. They explain how adjacent fluid layers slide relative to one another, connecting...
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Viscosity01:17

Viscosity

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When water is poured into a glass, it falls freely and quickly, whereas if honey or maple syrup is poured over a pancake, it flows slowly and sticks to the surface of the container. This difference in the flow of different kinds of liquids arises due to the fluid friction between the liquid layers and the liquid and the surrounding material. This property of fluids is called fluid viscosity. In this example, water has a lower viscosity than honey and maple syrup.
The SI unit of viscosity is...
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Related Experiment Video

Updated: Jun 9, 2025

Visually Based Characterization of the Incipient Particle Motion in Regular Substrates: From Laminar to Turbulent Conditions
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Visually Based Characterization of the Incipient Particle Motion in Regular Substrates: From Laminar to Turbulent Conditions

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Understanding density fluctuations in supersonic, isothermal turbulence.

Evan Scannapieco1, Liubin Pan2, Edward Buie3

  • 1School of Earth and Space Exploration, Arizona State University, 781 Terrace Mall, Tempe, AZ 85287, USA.

Science Advances
|October 30, 2024
PubMed
Summary
This summary is machine-generated.

Researchers modeled supersonic turbulence using tracer particles. The study reveals a balance between shock acceleration and stochastic processes shapes density distributions in astrophysical environments.

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Area of Science:

  • Astrophysics
  • Fluid Dynamics
  • Computational Physics

Background:

  • Supersonic turbulence is prevalent in astrophysical phenomena.
  • The probability density function (PDF) of logarithmic density in isothermal turbulence is empirically known but lacks theoretical explanation.
  • Understanding density distributions is key to modeling astrophysical environments.

Purpose of the Study:

  • To theoretically investigate the processes governing density distributions in supersonic turbulence.
  • To model the evolution of logarithmic density (s) and its derivative using stochastic processes.
  • To elucidate the mechanisms behind the observed density PDF in isothermal turbulence.

Main Methods:

  • Direct numerical simulations of supersonic turbulence.
  • Utilizing Lagrangian tracer particles to track density (s) and its derivative.
  • Developing a stochastic differential equation model with time-correlated noise.

Main Results:

  • The evolution of density and its derivative can be accurately modeled as a stochastic process with time-correlated noise.
  • Temporal correlation functions for density and its derivative exhibit exponential decay.
  • The model successfully explains conditional averages, indicating a balance between broadening (stochastic compressions/expansions) and narrowing (shock acceleration/deceleration) effects on the density PDF.

Conclusions:

  • A theoretical framework based on stochastic differential equations explains density PDF formation in supersonic turbulence.
  • The interplay between stochastic processes and shock dynamics is crucial for shaping density distributions.
  • The findings provide insights into the physics of turbulent astrophysical media.