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233814 results in Physics and Astronomy

Page 29 of 11691

  • 21 - Astrophysical and space applications

  • from Part 3 - From the Microscopic to Cosmic Scales
  • Ye Zhou, Lawrence Livermore National Laboratory, California
  • Book:
    Hydrodynamic Instabilities and Turbulence
    Published online:
    27 June 2024
    Print publication:
    19 December 2024, pp 442-456

  • Summary

    This chapter will provide a detailed presentation of the basic structure of the supernova and its core collapse process to illustrate the roles that RMI, RTI, and KHI play in the different stages of these processes. During the explosions, the shockwave passing through the onion-like supernova core will generate both RMI and RTI. The RTI is the key physical process creating the filament structures observed in the Crab Nebula. MHD RT instabilities will be presented to show how they can further improve the comparison between simulations and observations. Several additional applications where hydrodynamic instability plays an important role will also be examined. Geophysics and solar physics also present effective lenses to view the importance of hydrodynamic instabilities. In the case of solar physics, I will describe how RTI’s impact can be viewed through various phenomena, such as the plumes that rise from low density bubbles as well as eruptions that occur as material returns to the solar surface. Once again, MHD RT instabilities are relevant.

  • 13 - Reshock andmulti-shocks

  • from Part 2 - Hydrodynamics of Complex Flows
  • Ye Zhou, Lawrence Livermore National Laboratory, California
  • Book:
    Hydrodynamic Instabilities and Turbulence
    Published online:
    27 June 2024
    Print publication:
    19 December 2024, pp 247-276

  • Summary

    After the RM instability grows from a first shock, it can be hit by a second shock. These reshock scenarios have been found in the key applications of inertial confinement fusion implosions or supernova explosions. In this chapter, I will introduce the efforts to model the growth of the mixing layer induced by the first shock and subsequent reshock and describe how the turbulence kinetic energy and anisotropy might be affected by the reshock events. Data from shock tube experiments and numeric simulations will also be introduced to provide insight into the reshock RM induced flows.

  • 10 - Flow properties

  • from Part 2 - Hydrodynamics of Complex Flows
  • Ye Zhou, Lawrence Livermore National Laboratory, California
  • Book:
    Hydrodynamic Instabilities and Turbulence
    Published online:
    27 June 2024
    Print publication:
    19 December 2024, pp 183-213

  • Summary

    There are a number of microphysics and transport processes that can be extremely important to suppress or enhance the growth of these instabilities. I will provide a detailed description of how the hydrodynamic instability evolutions can be modified by incorporating the viscosity, surface tension, diffuse interface, and compressibility of the flows into the governing equations and growth rates.

Page 29 of 11691