Crushing of interstellar gas clouds in supernova remnants

Orlando, S.; Peres, G.; Reale, F.; Bocchino, F.; Rosner, R.; Plewa, T.; Siegel, A.

doi:10.1051/0004-6361:20052896

Cited by 112 publications

(155 citation statements)

References 39 publications

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“…It is clear from this figure that the KH instability does not play a significant role in the mass evolution. As found in Orlando et al (2005) the mass loss is dominated by evaporation off the cold cloud and not by hydrodynamic instabilities. Moreover, we see that in a few instances the lifetime of the clouds is longer when thermal conduction is switched on, contrary to what one might expect.…”

Section: Methodssupporting

confidence: 50%

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The Launching of Cold Clouds by Galaxy Outflows. Ii. The Role of Thermal Conduction

Brüggen

Scannapieco

2016

ApJ

130

123

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We explore the impact of electron thermal conduction on the evolution of radiatively cooled cold clouds embedded in flows of hot and fast material as it occurs in outflowing galaxies. Performing a parameter study of threedimensional adaptive mesh refinement hydrodynamical simulations, we show that electron thermal conduction causes cold clouds to evaporate, but it can also extend their lifetimes by compressing them into dense filaments. We distinguish between low column-density clouds, which are disrupted on very short times, and high-column density clouds with much longer disruption times that are set by a balance between impinging thermal energy and evaporation. We provide fits to the cloud lifetimes and velocities that can be used in galaxy-scale simulations of outflows in which the evolution of individual clouds cannot be modeled with the required resolution. Moreover, we show that the clouds are only accelerated to a small fraction of the ambient velocity because compression by evaporation causes the clouds to present a small cross-section to the ambient flow. This means that either magnetic fields must suppress thermal conduction, or that the cold clouds observed in galaxy outflows are not formed of cold material carried out from the galaxy.

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Section: Methodssupporting

confidence: 50%

“…The model most related to our current work is Orlando et al (2005). Using the same code as we do, the FLASH code, they investigated the competition between radiative cooling and thermal conduction during the evolution of spherical clouds exposed to a planar shock wave.…”

Section: Introductionmentioning

confidence: 99%

The Launching of Cold Clouds by Galaxy Outflows. Ii. The Role of Thermal Conduction

Brüggen

Scannapieco

2016

ApJ

130

123

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“…Observationally, there is also much evidence for cold gas being uplifted by buoyantly rising bubbles (Fabian et al 2003;Hatch et al 2006;Canning et al 2011;Werner et al 2013), suggesting that the cold gas does not simply feel the gravitational force, but has a response to the hydrodynamic forces from the hot gas. Second, there are no destruction mechanisms within our simulated clusters once the temperature of the cold gas drops below T=5×10 5 K. Therefore, the cold gas cannot be destroyed by shocks (Stone & Norman 1992;Klein et al 1994;Cooper et al 2009) or evaporated by thermal conduction (e.g., Orlando et al 2005Orlando et al , 2008, and thus the amount of cold gas obtained in the simulations (e.g., Figure 8) likely overestimates the actual value. Finally, our simulations are unable to follow the exact process of TI down to the Field length of the cold phase, which is far beyond the resolution of our simulations.…”

Section: Distribution Of Cold Gasmentioning

confidence: 85%

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

Yang

Reynolds

2016

ApJ

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Feedback from the active galactic nuclei (AGNs) is one of the most promising heating mechanisms to circumvent the cooling-flow problem in galaxy clusters. However, the role of thermal conduction remains unclear. Previous studies have shown that anisotropic thermal conduction in cluster cool cores (CCs) could drive the heat-flux-driven buoyancy instabilities (HBIs) that reorient the field lines in the azimuthal directions and isolate the cores from conductive heating from the outskirts. However, how the AGN interacts with the HBI is still unknown. To understand these interwined processes, we perform the first 3D magnetohydrodynamic simulations of isolated CC clusters that include anisotropic conduction, radiative cooling, and AGN feedback. We find the following: (1) For realistic magnetic field strengths in clusters, magnetic tension can suppress a significant portion of HBI-unstable modes, and thus the HBI is either completely inhibited or significantly impaired, depending on the unknown magnetic field coherence length. (2) Turbulence driven by AGN jets can effectively randomize magnetic field lines and sustain conductivity at ∼1/3 of the Spitzer value; however, the AGN-driven turbulence is not volumefilling. (3) Conductive heating within the cores could contribute to ∼10% of the radiative losses in Perseus-like clusters and up to ∼50% for clusters twice the mass of Perseus. (4) Thermal conduction has various impacts on the AGN activity and intracluster medium properties for the hottest clusters, which may be searched by future observations to constrain the level of conductivity in clusters. The distribution of cold gas and the implications are also discussed.

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“…A1a). The high effective temperatures of our main-sequence, massive stars produce a heat flux which timescale ∝ T −7/2 (Orlando et al 2005, Paper I) is much faster than both the dynamical advection timescale of the stellar wind and ISM gas in the bow shock and cooling by optically-thin radiative processes timescale. It transports large amount of the gas internal energy from the reverse shock of the bow shock towards the contact discontinuity that slightly enlarges the bow shock in the direction of motion of the star.…”

Section: Appendix A: the Effects Of Thermal Conductionmentioning

confidence: 93%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Crushing of interstellar gas clouds in supernova remnants

Cited by 112 publications

References 39 publications

The Launching of Cold Clouds by Galaxy Outflows. Ii. The Role of Thermal Conduction

The Launching of Cold Clouds by Galaxy Outflows. Ii. The Role of Thermal Conduction

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

Asymmetric supernova remnants generated by Galactic, massive runaway stars

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