The dynamics and high-energy emission of conductive gas clouds in supernova-driven galactic superwinds

Abstract

Superwinds from starburst galaxies are multiphase outflows that sweep up and incorporate ambient galactic disc and halo gas. The interaction of this denser material with the more diffuse hot wind gas is thought to give rise to the O VI emission and absorption in the far ultraviolet (FUV) and the soft thermal X-ray emission observed in superwinds. In this paper, we present high-resolution hydrodynamical models of warm ionized clouds embedded in a superwind, and compare the O VI and soft X-ray properties to the existing observational data. These models include thermal conduction, which we show plays an important role in shaping both the dynamics and radiative properties of the resulting wind/cloud interaction. Heat conduction stabilizes the cloud by inhibiting the growth of Kelvin-Helmholtz and Rayleigh-Taylor instabilities, and also generates a shock wave at the cloud's surface that compresses the cloud. This dynamical behaviour influences the observable properties. We find that while O VI emission and absorption always arises in cloud material at the periphery of the cloud, most of the soft X-ray arises in the region between the wind bow shock and the cloud surface, and probes either wind or cloud material depending on the strength of conduction and the relative abundances of the wind with respect to the cloud. In general, only a small fraction ( 1 per cent) of the wind mechanical energy intersecting a cloud is radiated away at ultraviolet (UV) and X-ray wavelengths, with more wind energy going into accelerating the cloud. Clouds in relatively slow cool winds radiate a larger fraction of their energy, which are inconsistent with observational constraints. Models with heat conduction at Spitzer-levels are found to produce observational properties closer to those observed in superwinds than models with no thermal conduction, in particular, in terms of the O VI to X-ray luminosity ratio, but cloud life times are uncomfortably short ( 1 Myr) compared to the dynamical ages of real winds. We experimented with reducing the thermal conductivity for one set of model parameters, and found that even when we reduced conduction by a factor of 25 that the simulations retained the beneficial hydrodynamical stability and low O VI to X-ray luminosity ratio found in the Spitzer-level conductive models, while also having reduced evaporation rates. Although more work is required to simulate clouds for longer times and to investigate cloud acceleration and thermal conduction at sub-Spitzer levels in a wider range of models, we conclude that thermal conduction can no longer be ignored in superwinds.

PHYSICAL CONDITIONS IN THE LOW-IONIZATION COMPONENT OF STARBURST OUTFLOWS: THE SHAPE OF NEAR-ULTRAVIOLET AND OPTICAL ABSORPTION-LINE TROUGHS IN KECK SPECTRA OF ULIRGs

“…A close connection likely exists between this neutral-atomic gas, outflowing dust, and large-scale molecular outflows. Images revealing the presence of dust and molecular gas in M82 out to a few kpc (Walter et al 2002;Hoopes et al 2005;Veilleux et al 2009b) provide strong evidence for the survival (or continuous creation) of dense clouds despite ablation by the hot wind and evaporation, as described (for example) by Marcolini et al (2005).…”

Dust destruction in the ISM: a re-evaluation of dust lifetimes

“…From the observational results discussed in Sect. 4.3 it appears that in shocked environments matter is entrained into shock-formed or shock-enhanced clumps, as observed in stellar and galactic winds expanding into inhomogenous media (e.g., Chevalier & Clegg 1985;Suchkov et al 1994;Strickland & Stevens 2000;Marcolini et al 2005, see also the discussion in Sect. 4.3).…”

Extreme Feedback and the Epoch of Reionization: Clues in the Local Universe

“…Steidel et al (2010) find line centroids that are blueshifted on-average by 164 km s −1 and maximum outflow speeds that are typically ∼800 km s −1 for galaxies with star formation rates of ∼10 1 -10 2 M yr −1 . Outflows from intensely star-forming galaxies are believed to be produced as gas clouds are accelerated by the ram pressure of a hot and fast wind driven by the collective thermal/kinetic energy supplied by supernovae and massive stellar winds (e.g., Heckman et al 2000;Veilleux et al 2005;Marcolini et al 2005), and/or by radiation pressure acting on dust (Murray et al 2005(Murray et al , 2010. Can the unusually high velocities seen in the DCOs be explained in this way?…”

“…One plausible physical model would be that the neutral gas represents the denser cores of clouds being accelerated by the wind, while the ionized gas represents a lower density halo of gas and dust surrounding the cloud core and which is being ablated by the wind and photoionized by the intense radiation field (e.g., Marcolini et al 2005).…”