Stellar wind termination shocks in massive clusters have structure determined solely by the surrounding cavity's density and pressure, enabling efficient modeling of arbitrary cluster ages and producing spherical shocks in 5 Myr old systems.
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The high-contrast dust asymmetry in HD 34700A is reproduced by a vortex model, with contrast levels excluding eccentric cavity orbit clustering.
Radiative cooling thins hot accretion disks around black holes, reduces wind power, and makes inflow-rate decrease depend more on MRI-driven turbulence than on winds as cooling strengthens.
citing papers explorer
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How interacting winds shape the mechanical feedback of massive star clusters over millions of years
Stellar wind termination shocks in massive clusters have structure determined solely by the surrounding cavity's density and pressure, enabling efficient modeling of arbitrary cluster ages and producing spherical shocks in 5 Myr old systems.
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The Circumbinary Disc of HD 34700A II. Analysis of a strong dust asymmetry
The high-contrast dust asymmetry in HD 34700A is reproduced by a vortex model, with contrast levels excluding eccentric cavity orbit clustering.
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Radiative cooling effects on black hole hot accretion flows around the sub-Bondi radius
Radiative cooling thins hot accretion disks around black holes, reduces wind power, and makes inflow-rate decrease depend more on MRI-driven turbulence than on winds as cooling strengthens.