Three-Dimensional Simulations of a Starburst-driven Galactic Wind

By Jackie L. Cooper, G. Bicknell, R. Sutherland, Joss Bland-Hawthorn. 2008

153 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/6446cb2090a2e41370299c8457116d2b656df4a5

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In Astronomy and Astrophysics

Citations in the corpus

THE SYSTEMATIC PROPERTIES OF THE WARM PHASE OF STARBURST-DRIVEN GALACTIC WINDS (2015, background): “…et al. 2015; Henriques et al. 2015; Mitra et al. 2015), high-resolution simulations of individual galaxies that are able to calculate ab initio more of the relevant physical processes are clearly needed (e.g. Cooper et al. 2008, 2009; Shen et al. 2013; Hopkins et al. 2013; Muratov et al. 2015).”
Lyα Emitting Galaxies as a Probe of Reionisation (2014, methodology): “This requires (magneto)hydrodynamical simulations with sub-pc resolution (e.g. Cooper et al. 2008; Fujita et al. 2009).”
DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, background): “The low-ionization gas is entrained in the hot wind by the breakup of supershells (Fujita et al. 2009), the shear between the free wind and the galactic ISM (Heckman et al. 2000), and pre-existing, interstellar clouds (Cooper et al. 2008, 2009).”
THE SINS SURVEY OF z ∼ 2 GALAXY KINEMATICS: PROPERTIES OF THE GIANT STAR-FORMING CLUMPS (2010, background): “…a stratified disk, the bubble will expand preferentially along the minor axis of the disk, and will eventually “blow out” into the halo, although the magnitude and appearance of this blow out may be strongly modified and lowered in a strongly inhomogeneous interstellar medium (Cooper et al. 2008).”
Relativistic jet feedback – III. Feedback on gas discs (2018, background): “16 the inclined jets launch a vertical outflow that creates a super bubble with a morphology usually expected from a nuclear star burst driven bubble (Veilleux et al. 2005; Cooper et al. 2008; Vijayan et al. 2018).”
RADIATION PRESSURE FROM MASSIVE STAR CLUSTERS AS A LAUNCHING MECHANISM FOR SUPER-GALACTIC WINDS (2010, background): “As numerous authors have pointed out, in such a scenario the cold gas is subject to Kelvin-Helmholtz instabilities (Klein et al. 1994; Cooper et al. 2008) and/or by conductive evaporation (Marcolini et al. 2005) and ends up surviving for less than 1Myr (a few cloud crushing times) before being…”
THREE-DIMENSIONAL INTEGRAL FIELD OBSERVATIONS OF 10 GALACTIC WINDS. I. EXTENDED PHASE (≳10 Myr) OF MASS/ENERGY INJECTION BEFORE THE WIND BLOWS (2010, background): “The connection between the evaporating cloud skins and the intracloud wind material may help the wind to entrain denser gas from these same clouds (Cooper et al. 2008).”