tokens: model are included here for completeness. We employ a predictor–corrector integration method based on the description in Stone Gardiner ( 2009 ), along with a second-order spatial reconstruction technique with limiting applied in the characteristic variables (LeVeque 2002 ) and the HLLC Riemann solver (Toro et al. 1994 ; Batten et al. 2006 ). Radiative cooling is included via operator splitting, with the thermal energy losses accounted for after the hydrodynamic update. The cooling rates are determined using a forward Euler integration, and subcycling of the radiative cooling time step is employed to ensure a numerically robust solution. The cooling function is a piecewise parabolic fit to a solar-metallicity, collisional ionization equilibrium curve calculated using Cloudy (Ferland et al. 2013 ). Cooling is only included for gas above 10 4 K; below this cutoff a temperature floor is assumed for all the gas in the simulation. The cutoff is primarily employed to prevent collapse of the isothermal gas disk, but we note that the rarefied gas in the outflow will be subject to photoionization heating from the cosmic UV background and therefore would not be expected to cool much below 10 4 K (see Schneider Robertson 2017 ). Photoionization heating is not explicitly included in these simulations. All of the gas in the simulations is assumed to be ionized, with an adiabatic index γ = 5/3 and a mean molecular weight μ = 0.6 used in all calculations and analysis. 3. Results We begin our results by presenting a phenomenological description of the three high-resolution simulations: the central feedback model without cooling (Model A), the central feedback model with cooling (Model B), and the clustered feedback model with cooling (Model C). As explained in Section 2 , the only difference between Models A and B is the inclusion of radiative cooling in the simulation. Model A therefore represents a 3D numerical test of the original CC85 analytic model with the inclusion of a galactic disk. Similarly, Model B can be directly related to the Thompson et al. ( 2016 ) outflow model that accounts for radiative energy losses. A comparison between Figures 1 and 2 shows the dramatic effect that radiative cooling can have on the overall character of a mass-loaded outflow. In these figures, we plot density, radial velocity, and temperature slices in the centered x − z plane. Some features are common to both simulations—namely, the 10 4 K disk and the spherical gain region at the center where mass and energy are injected. In Model A, a biconical free-wind region is clearly visible in both the density and temperature slices, surrounded by a region of more turbulent, higher-temperature gas where the outflow is interacting with the disk gas. In Model B, turbulence at the disk–outflow interface is highly suppressed, leading to a free-wind region with opening angle nearly ΔΩ = 4 π . Although energy is injected into the hot wind at the same rate in Models A and B, the
ner_tags: O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O B-Citation I-Citation O O O B-Software I-Software I-Software B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-EntityOfFutureInterest O O O O O O B-Software B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O O O O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model I-Model I-Model I-Model B-Citation I-Citation O B-Model I-Model I-Model I-Model I-Model B-Model I-Model O O B-Model I-Model I-Model I-Model I-Model B-Model I-Model O O O O O O O O O O B-Model I-Model O B-Model O O O O O O O O O B-Model I-Model O O O O O O O O B-Model I-Model I-Model I-Model O O O O O O O O B-Model I-Model O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O B-Citation I-Citation O B-Citation O