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.
Monthly Notices of the Royal Astronomical Society474(2), 2212–2232 (2018)
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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.
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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.
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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.