Propagation of blast waves

Supernova (SN) blast waves inject energy and momentum into the interstellar medium (ISM), control its turbulent multiphase structure and the launching of galactic outflows. Accurate modelling of the blast wave evolution is therefore essential for ISM and galaxy formation simulations. We present an efficient method to compute the input of momentum, thermal energy, and the velocity distribution of the shock-accelerated gas for ambient media (densities of 0.1 n 0 [cm −3 ] 100) with uniform (and with stellar wind blown bubbles), power-law, and turbulent (Mach numbers M from 1 − 100) density distributions. Assuming solar metallicity cooling, the blast wave evolution is followed to the beginning of the momentum conserving snowplough phase. The model recovers previous results for uniform ambient media. The momentum injection in wind-blown bubbles depend on the swept-up mass and the efficiency of cooling, when the blast wave hits the wind shell. For power-law density distributions with n(r) ∼ r −2 (for n(r) > n floor ) the amount of momentum injection is solely regulated by the background density n floor and compares to n uni = n floor . However, in turbulent ambient media with log-normal density distributions the momentum input can increase by a factor of 2 (compared to the homogeneous case) for high Mach numbers. The average momentum boost can be approximated as . The velocity distributions are broad as gas can be accelerated to high velocities in low-density channels. The model values agree with results from recent, computationally expensive, three-dimensional simulations of SN explosions in turbulent media.

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“…The expansion speed can be derived by considering the time derivatives of the shock radius r S in the ST stage (Cavaliere & Messina 1976):…”

Section: Sedov-taylor Phasementioning

confidence: 99%

“…(21) Without this lower limit the mean of the ambient density would drop to non-physical values and the sound speed of the ambient medium with a fixed pressure would increase to infinity (Chevalier 1976;Cavaliere & Messina 1976;Greif et al 2011;Hennebelle & Falgarone 2012).…”

Section: The Numerical Setupmentioning

confidence: 99%

Supernova blast waves in wind-blown bubbles, turbulent, and power-law ambient media

Haid

Walch

Naab

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The fraction is when the medium is constituted by relativistic particles 1 a ≈ 2 (see Cavaliere & Messina 1976), and in the case of a a p 1 thermalized superwind.…”

Section: No 1 2006 Searching For Agn-driven Shocks In Galaxy Clustementioning

confidence: 99%

Searching for AGN-driven Shocks in Galaxy Clusters

Cavaliere

Lapi

2006

ApJ

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Shocks and blast waves are conceivably driven into the intracluster medium filling galaxy groups and clusters by powerful outbursts of active galactic nuclei or quasars in the member galaxies; the first footprints of shock fronts have been tentatively traced out with X-ray imaging. We show how overpressures in the blasts behind the shock can prove the case and also provide specific marks of the nuclear activity: its strength, its current stage, and the nature of its prevailing output. We propose to detect these marks with the aimed pressure probe constituted by the resolved Sunyaev-Zel'dovich effect. We compute and discuss the outcomes to be expected in nearby and distant sources at different stages of their activity.

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“…shock , respectively, with t the time (Cavaliere & Messina, 1976). The previous expressions have been proposed by Smart & Shea (1985) 14:00 00:00 10:00 20:00 06:00 16:00 Start Time ( Cavaliere & Messina (1976).…”

Section: Comparison With Observationsmentioning

confidence: 99%

“…The previous expressions have been proposed by Smart & Shea (1985) 14:00 00:00 10:00 20:00 06:00 16:00 Start Time ( Cavaliere & Messina (1976). The driving standoff distance and the CME radius were calculated using the models of Farris & Russell (1994) and Bothmer & Schwenn (1998), respectively.…”

Section: Comparison With Observationsmentioning

confidence: 99%

Dynamic evolution of interplanetary shock waves driven by CMEs

Corona‐Romero

González-Esparza

2011

Proc. IAU

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Abstract. We present a study about the propagation of interplanetary shock waves driven by super magnetosonic coronal mass ejections (CMEs). The discussion focuses on a model which describes the dynamic relationship between the CME and its driven shock and the way to approximate the trajectory of shocks based on those relationships, from near the Sun to 1 AU. We apply the model to the analysis of a case study in which our calculations show quantitative and qualitative agreements with different kinds of data. We discuss the importance of solar wind and CME initial conditions on the shock wave evolution.

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Propagation of blast waves

Cited by 30 publications

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Supernova blast waves in wind-blown bubbles, turbulent, and power-law ambient media

Supernova blast waves in wind-blown bubbles, turbulent, and power-law ambient media

Searching for AGN-driven Shocks in Galaxy Clusters

Dynamic evolution of interplanetary shock waves driven by CMEs

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