Mach number study of supersonic turbulence: The properties of the density field

TL;DR

This study investigates how the properties of the density field in supersonic turbulence vary with Mach number, revealing specific scaling relations, spectral behaviors, and fractal dimensions across a wide Mach number range.

Contribution

It provides new quantitative relations for density fluctuations and spectral scaling in supersonic turbulence, including the dependence of spectral exponents on Mach number and a novel fitting formula for density spectra.

Findings

Density fluctuations follow a specific log-normal relation with Mach number.

Density spectra exhibit Mach-dependent power-law scaling and curvature.

The fractal dimension decreases with increasing Mach number.

Abstract

We model driven, compressible, isothermal, turbulence with Mach numbers ranging from the subsonic ($\mathcal{M} \approx 0.65$) to the highly supersonic regime ($\mathcal{M}\approx 16 $). The forcing scheme consists both solenoidal (transverse) and compressive (longitudinal) modes in equal parts. We find a relation $\sigma_{s}^2 = \mathrm{b}\log{(1+\mathrm{b}^2\mathcal{M}^2)}$ between the Mach number and the standard deviation of the logarithmic density with $\mathrm{b} = 0.457 \pm 0.007$. The density spectra follow $\mathcal{D}(k,\,\mathcal{M}) \propto k^{\zeta(\mathcal{M})}$ with scaling exponents depending on the Mach number. We find $\zeta(\mathcal{M}) = \alpha \mathcal{M}^{\beta}$ with a coefficient $\alpha$ that varies slightly with resolution, whereas $\beta$ changes systematically. We extrapolate to the limit of infinite resolution and find $\alpha = -1.91 \pm 0.01,\, \beta =-0.30\pm 0.03$. The dependence of the scaling exponent on the Mach number implies a fractal dimension $D=2+0.96 \mathcal{M}^{-0.30}$. We determine how the scaling parameters depend on the wavenumber and find that the density spectra are slightly curved. This curvature gets more pronounced with increasing Mach number. We propose a physically motivated fitting formula $\mathcal{D}(k) = \mathcal{D}_0 k^{\zeta k^{\eta}}$ by using simple scaling arguments. The fit reproduces the spectral behaviour down to scales $k\approx 80$. The density spectrum follows a single power-law $\eta = -0.005 \pm 0.01$ in the low Mach number regime and the strongest curvature $\eta = -0.04 \pm 0.02$ for the highest Mach number. These values of $\eta$ represent a lower limit, as the curvature increases with resolution.