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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Resolving the inner few AU in protostellar disk simulations yields complete tidal disruption of migrating fragments and shorter, sharper accretion outbursts than coarser 30 AU models.
Simulations demonstrate that mega-parsec giant radio sources form successfully in normal hot baryonic gas environments within 10^13 to 10^15 solar mass dark matter halos, with radio powers matching observations.
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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From Fragments to Flares: Migration, Tidal Disruption, and Observable Bursts in Massive Protostellar Disks
Resolving the inner few AU in protostellar disk simulations yields complete tidal disruption of migrating fragments and shorter, sharper accretion outbursts than coarser 30 AU models.
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Formation of mega-parsec giant radio sources from hosts residing in dark matter halos with normal hot baryonic gas fractions
Simulations demonstrate that mega-parsec giant radio sources form successfully in normal hot baryonic gas environments within 10^13 to 10^15 solar mass dark matter halos, with radio powers matching observations.
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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.