A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.
The Astrophysical Journal891(2), 154 (2020)
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
citation-role summary
background 2
citation-polarity summary
years
2026 3roles
background 2polarities
background 2representative citing papers
Turbulent torques modeled as a Gaussian around the linear torque can push gas-induced dephasing in LISA EMRIs above the detection threshold for Eddington ratios above 0.3 and sufficient turbulence strength.
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
citing papers explorer
-
The slope of the power spectrum of the density field in isothermal supersonic compressible turbulence
A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.
-
Chaotic migration of LISA Extreme Mass Ratio Inspirals in a turbulent accretion disk: effect on waveform de-phasing
Turbulent torques modeled as a Gaussian around the linear torque can push gas-induced dephasing in LISA EMRIs above the detection threshold for Eddington ratios above 0.3 and sufficient turbulence strength.
-
Giant Planet Formation by Disk Instability
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.