The growth and entrainment of cold gas in a hot wind

Grönke, Max; Oh, S. Peng

doi:10.1093/mnrasl/sly131

Cited by 287 publications

(320 citation statements)

References 28 publications

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“…What drives coagulation? There are at least two causes: (i) radiative cooling, which drives pressure gradients in mixed interstitial gas, the source of mass growth discussed in Gronke & Oh (2018. Cooling-induced coalescence has also been highlighted in Elphick et al (1991); Waters & Proga (2019), though merger velocities seen in those 1D (i.e., no turbulence or mixing), low overdensity (χ ∼ few) calculations are much smaller than seen there, and could not compete with breakup.…”

Section: Discussionmentioning

confidence: 99%

Is multiphase gas cloudy or misty?

Grönke

2020

Monthly Notices of the Royal Astronomical Society: Letters

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Cold T ∼ 10 4 K gas morphology could span a spectrum ranging from large discrete clouds to a fine 'mist' in a hot medium. This has myriad implications, including dynamics and survival, radiative transfer, and resolution requirements for cosmological simulations. Here, we use 3D hydrodynamic simulations to study the pressure-driven fragmentation of cooling gas. This is a complex, multi-stage process, with an initial Rayleigh-Taylor unstable contraction phase which seeds perturbations, followed by a rapid, violent expansion leading to the dispersion of small cold gas 'droplets' in the vicinity of the gas cloud. Finally, due to turbulent motions, and cooling, these droplets may coagulate. Our results show that a gas cloud 'shatters' if it is sufficiently perturbed out of pressure balance (δP/P ∼ 1), and has a large final overdensity χ f 300, with only a weak dependence on the cloud size. Otherwise, the droplets reassemble back into larger pieces. We discuss our results in the context of thermal instability, and clouds embedded in a shock heated environment.

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Section: Discussionmentioning

confidence: 99%

Is multiphase gas cloudy or misty?

Grönke

2020

Monthly Notices of the Royal Astronomical Society: Letters

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“…Moreover, cloud-scale high resolution simulations of cold clumps embedded in a hot medium with realistic conditions for the stripped tails will be fundamental to assess the hypothesis proposed in this paper and analyze the various possibilities for ISM heating (e.g. Brüggen & Scannapieco (2016); Armillotta et al (2016); Gronke & Oh (2018)).…”

Section: The Heating Ism Scenario and The Hα-x-ray Correlationmentioning

confidence: 99%

GASP XXIII: A Jellyfish Galaxy as an Astrophysical Laboratory of the Baryonic Cycle

Poggianti

Ignesti

Gitti

et al. 2019

ApJ

107

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With MUSE, Chandra, VLA, ALMA and UVIT data from the GASP programme we study the multiphase baryonic components in a jellyfish galaxy (JW100) with a stellar mass 3.2 × 10 11 M hosting an AGN. We present its spectacular extraplanar tails of ionized and molecular gas, UV stellar light, X-ray and radio continuum emission. This galaxy represents an excellent laboratory to study the interplay between different gas phases and star formation, and the influence of gas stripping, gas heating, and AGN. We analyze the physical origin of the emission at different wavelengths in the tail, in particular in-situ star formation (related to Hα, CO and UV emission), synchrotron emission from relativistic electrons (producing the radio continuum) and heating of the stripped interstellar medium (ISM) (responsible for the X-ray emission). We show the similarities and differences of the spatial distributions of ionized gas, molecular gas and UV light, and argue that the mismatch on small scales (1kpc) is due to different stages of the star formation process. We present the relation Hα-X-ray surface brightness, which is steeper for star-forming regions than for diffuse ionised gas regions with high [OI]/Hα ratio. We propose that ISM heating due to interaction with the intracluster medium (either for mixing, thermal conduction or shocks) is responsible for the X-ray tail, the observed [OI]excess and the lack of star formation in the northern part of the tail. We also report the tentative discovery in the tail of the most distant (and among the brightest) currently known ULX, a point-like ultraluminous X-ray source commonly originating in a binary stellar system powered either by an intermediate-mass black hole or a magnetized neutron star.

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“…The other possibility is that we underestimate the ability of AGN feedback to destroy dense clumps, for example by underresolving the mixing layers at the outer clump surface (Gronke & Oh 2018), or simply due to lack of resolution to follow the fragmentation process to smaller scales. This hypothesis is supported by our high-resolution companion simulation, which showed that the fraction of dense gas that survives this particular uplifting event falls from 25 % at a resolution of ∆x min = 120 pc to 19 % at a resolution of ∆x min = 30 pc.…”

Section: Filament Lifetimesmentioning

confidence: 99%

Dense gas formation and destruction in a simulated Perseus-like galaxy cluster with spin-driven black hole feedback

Beckmann

Dubois

Guillard

et al. 2019

A&A

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Context. Extended filamentary Hα emission nebulae are a striking feature of nearby galaxy clusters but the formation mechanism of the filaments, and the processes which shape their morphology remain unclear. Aims. We conduct an investigation into the formation, evolution and destruction of dense gas in the center of a simulated, Perseus-like, cluster under the influence of a spin-driven jet. The jet is powered by the supermassive black hole located in the cluster's brightest cluster galaxy. We particularly study the role played by condensation of dense gas from the diffuse intracluster medium, and the impact of direct uplifting of existing dense gas by the jets, in determining the spatial distribution and kinematics of the dense gas. Methods. We present a hydrodynamical simulation of an idealised Perseus-like cluster using the adaptive mesh refinement code ramses. Our simulation includes a supermassive black hole (SMBH) that self-consistently tracks its spin evolution via its local accretion, and in turn drives a large-scale jet whose direction is based on the black hole's spin evolution. The simulation also includes a live dark matter (DM) halo, a SMBH free to move in the DM potential, star formation and stellar feedback. Results. We show that the formation and destruction of dense gas is closely linked to the SMBH's feedback cycle, and that its morphology is highly variable throughout the simulation. While extended filamentary structures readily condense from the hot intracluster medium, they are easily shattered into an overly clumpy distribution of gas during their interaction with the jet driven outflows. Condensation occurs predominantly onto infalling gas located 5 -15 kpc from the center during quiescent phases of the central AGN, when the local ratio of the cooling time to free fall time falls below 20, i.e. when t cool /t ff < 20. Conclusions. We find evidence for both condensation and uplifting of dense gas, but caution that purely hydrodynamical simulations struggle to effectively regulate the cluster cooling cycle and produce overly clumpy distributions of dense gas morphologies, compared to observation.

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The growth and entrainment of cold gas in a hot wind

Cited by 287 publications

References 28 publications

Is multiphase gas cloudy or misty?

Is multiphase gas cloudy or misty?

GASP XXIII: A Jellyfish Galaxy as an Astrophysical Laboratory of the Baryonic Cycle

Dense gas formation and destruction in a simulated Perseus-like galaxy cluster with spin-driven black hole feedback

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