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Simulations, Data Analysis and Algorithms

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Figure 3 | Computational Astrophysics and Cosmology

Figure 3

From: Implicit large eddy simulations of anisotropic weakly compressible turbulence with application to core-collapse supernovae

Figure 3

Energy flux, as defined by equation ( 16 ), obtained with different numerical methods and resolutions. The energy flux is shown normalized to the average dissipation rate given by equation (24). From left to right and from top to bottom we show the results obtained with PPM_HLLC, PPM_HLLC_CFL0.8, PPM_HLLE, TVD_HLLE and WENOZ_HLLC. The bottom right panel show a comparison of all of the methods at 5123. All of the schemes show a good level of accuracy in the energy flux from the largest scales, with errors smaller than a few % already at low resolutions. The differences between the schemes become more marked at large wave numbers where the numerical dissipation starts to interfere with the energy cascade.

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