Assess the impact of a more comprehensive physical model

Assess how incorporating the full energy equation and alternative driving mechanisms, as in the simulations of compressible turbulence reported by JDSJFM2021, affects the two Mach-number-dependent dissipative-anomaly branches and their asymptotic behavior.

Background

The present study considers an isothermal equation of state and purely solenoidal forcing. The authors contrast this setup with earlier simulations that included the full energy equation and different ways of driving the turbulence.

The comparison is relevant because thermodynamic evolution and forcing type may alter the production mechanisms, spatial organization, and Reynolds-number dependence of total, solenoidal, and dilatational dissipation. The paper explicitly states that the consequences of this more comprehensive physical model cannot be evaluated within the present work.

References

A direct measurement of the compressible energy transfer, through the density-weighted variable $\rho{1/3}\boldsymbol{v}$ \citep{2007ApJ...665..416Kritsuk} or the exact compressible flux law \citep{2011PhRvL.107m4501Galtier}, is left to future work.

— The WEFT project: I. The emergence of turbulence in a cosmic filament  (2609.17205 - Lebeau et al., 15 Sep 2026) in Section 6, “From shock-dominated intermittency to a developed cascade”

The impact of this more comprehensive physical model remains to be understood and cannot be assessed within the present work.

— Mach-number-dependent dissipative anomaly in isothermal compressible turbulence  (2609.03945 - Alam et al., 3 Sep 2026) in Section 8, Summary and outlook

This indication should nevertheless be taken with caution: simulations cannot reproduce the Reynolds numbers, the range or the expansion of the solar wind plasma, and the relative weight of the source and hybrid terms in the interplanetary medium remains essentially unconstrained observationally.

— Effects of Alfvénicity on the Compressible Energy Cascade in Magnetohydrodynamic Solar Wind Turbulence: Evidence from Parker Solar Probe, Solar Orbiter, and WIND observations  (2609.37856 - Andrés et al., 29 Sep 2026) in Section 3, The Energy Cascade Rate at MHD Scales