The slope of the power spectrum of the density field in isothermal supersonic compressible turbulence
Fuente:
arXiv
Salvato in:
| Autori principali: | , , , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2026
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866909030672236544 |
|---|---|
| author | Dumond, Pierre Fensch, Jérémy Chabrier, Gilles Brucy, Noé |
| author_facet | Dumond, Pierre Fensch, Jérémy Chabrier, Gilles Brucy, Noé |
| contents | The power spectrum (PS) of the density field in supersonic turbulence is a fundamental quantity that characterizes the statistical properties of the structures formed in compressible flows. It is also widely used to estimate the Mach number in the interstellar medium from simulation-derived relations. In this paper, we provide a first quantitative explanation for the evolution of the slope of the PS of the density field with the Mach number in homogeneous isotropic isothermal turbulence using a time-invariant quantity derived by Chandrasekhar (1951). For simulated turbulent flows, the model reproduces the measured slopes for different widths of the inertial range and density variances very well. Our model also provides a comprehensive interpretation of the characteristic slopes of the PS of the density field measured in the interstellar medium. Based on these results, we stress that the Mach number cannot be reliably deduced from the slope of the PS of the density field. In closing, we discuss a resolution criterion that must be fulfilled to correctly simulate a turbulent flow with a given density PS slope. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2605_03924 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | The slope of the power spectrum of the density field in isothermal supersonic compressible turbulence Dumond, Pierre Fensch, Jérémy Chabrier, Gilles Brucy, Noé Astrophysics of Galaxies Solar and Stellar Astrophysics Fluid Dynamics The power spectrum (PS) of the density field in supersonic turbulence is a fundamental quantity that characterizes the statistical properties of the structures formed in compressible flows. It is also widely used to estimate the Mach number in the interstellar medium from simulation-derived relations. In this paper, we provide a first quantitative explanation for the evolution of the slope of the PS of the density field with the Mach number in homogeneous isotropic isothermal turbulence using a time-invariant quantity derived by Chandrasekhar (1951). For simulated turbulent flows, the model reproduces the measured slopes for different widths of the inertial range and density variances very well. Our model also provides a comprehensive interpretation of the characteristic slopes of the PS of the density field measured in the interstellar medium. Based on these results, we stress that the Mach number cannot be reliably deduced from the slope of the PS of the density field. In closing, we discuss a resolution criterion that must be fulfilled to correctly simulate a turbulent flow with a given density PS slope. |
| title | The slope of the power spectrum of the density field in isothermal supersonic compressible turbulence |
| topic | Astrophysics of Galaxies Solar and Stellar Astrophysics Fluid Dynamics |
| url | https://arxiv.org/abs/2605.03924 |