Analytic theory for transmission spectra of hydrodynamic planetary outflows identifies an opacity-mass-loss saturation boundary beyond which escape rates cannot be uniquely recovered from spectral lines.
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Simulations show high-speed solar wind streams evolve via interactions and 3D flows, making them non-parcel-preserving and location-dependent in their observed properties.
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.
citing papers explorer
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A theory of transmission spectroscopy of hydrodynamic outflows from planetary atmospheres: Spectral-line saturation and limits on mass-loss constraints
Analytic theory for transmission spectra of hydrodynamic planetary outflows identifies an opacity-mass-loss saturation boundary beyond which escape rates cannot be uniquely recovered from spectral lines.
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MHD simulations on the large-scale propagation of high-speed solar wind streams
Simulations show high-speed solar wind streams evolve via interactions and 3D flows, making them non-parcel-preserving and location-dependent in their observed properties.
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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.