August 7-10, 2017


Radiation Transport Through Super-Eddington Stellar Winds in Luminous Stars

Joyce A. Guzik (Los Alamos National Laboratory)

Chris Fryer, Todd Urbatsch (Los Alamos National Laboratory), Stanley Owocki (University of Delaware)

We explore the consequences for eruptive mass loss in massive stars that may be driven by an abrupt high energy-deposition rate in the interior. This energy deposition could be initiated by, e.g., gravity waves or binary merger and common envelope evolution. These mechanisms have been proposed to explain the enhanced mass loss during giant eruptions of luminous blue variables (LBVs) and in pre-supernova events. The radiation flow and hydrodynamics may cause the outer layers to break up into clumps or become ‘porous’, reducing the effect of radiation driving and changing stellar wind properties and other observational characteristics. 3-D hydrodynamic models with radiation transport methods that are more sophisticated than radiation diffusion will be needed to model the outcome. Here we present modeling of this problem using the 3-D Los Alamos code Cassio, an adaptive grid radiation hydrodynamics code that includes implicit Monte Carlo radiation transport. This code is capable in principle of modeling both radiative and convective energy transport, and accounting for radiation flow through inhomogeneous clumps and density gradients created from outflow and subsequent fallback. We present the first results of 1-D models, and compare results with the analytical work of Owocki, Townsend and Quataert (2017, MNRAS, submitted) and prior 1-D simulations

Mode of presentation: poster