Winds Driven by Super Star Clusters: The Self‐Consistent Radiative Solution

Silich, Sergiy; Tenorio-Tagle, G.; Rodríguez-González, A.

doi:10.1086/421702

Cited by 141 publications

(230 citation statements)

References 24 publications

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“…The last three parameters are the new ingredients incorporated in our formulation. When Ve = 0, α = 0 and A → ∞ we recover the radiative threshold lines for the standard CC85 model estimated first numerically by Silich, Tenorio-Tagle & Rodríguez-González (2004), given analytically by Añorve-Zeferino (2006) using a necessary and sufficient condition for the existence of the stationary flow, and generalized later semi-analytically by Wünsch et al (2007) for CC85-like bimodal outflows. We are also able to reproduce as a particular case the threshold lines numerically obtained by Silich et al (2010) for a uniform distribution including the gravitational field (Ve = 0, α = 0 and A → ∞).…”

Section: (B4)supporting

confidence: 74%

Gravitational and mass distribution effects on stationary superwinds

Añorve-Zeferino¹

2016

Mon. Not. R. Astron. Soc.

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Here, we model the effect of non-uniform dynamical mass distributions and their associated gravitational fields on the stationary galactic superwind solution. We do this by considering an analogue injection of mass and energy from stellar winds and SNe. We consider both compact dark-matter and baryonic haloes that does not extend further from the galaxies optical radii R opt as well as extended gravitationally-interacting ones. We consider halo profiles that emulate the results of recent cosmological simulations and coincide also with observational estimations from galaxy surveys. This allows to compare the analytical superwind solution with outflows from different kinds of galaxies. We give analytical formulae that establish when an outflow is possible and also characterize distinct flow regimes and enrichment scenarios. We also constraint the parameter space by giving approximate limits above which gravitation, self-gravitation and radiative cooling can inhibit the stationary flow. We obtain analytical expressions for the free superwind hydrodynamical profiles. We find that the existence or inhibition of the superwind solution highly depends on the steepness and concentration of the dynamical mass and the mass and energy injection rates. We compare our results with observational data and a recent numerical work. We put our results in the context of the mass-metallicity relationship to discuss observational evidence related to the selective loss of metals from the least massive galaxies and also discuss the case of massive galaxies.

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Section: (B4)supporting

confidence: 74%

Gravitational and mass distribution effects on stationary superwinds

Añorve-Zeferino¹

2016

Mon. Not. R. Astron. Soc.

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“…The presence of the BH does not affect the relation between the gas number density and the temperature at the stagnation point found in Silich et al (2004):…”

Section: Scmentioning

confidence: 89%

“…[9] and [12]) the sonic point (the point where the outflow velocity is equal to the local speed of sound) to be located at the star cluster surface (see Cantó et al 2000;Silich et al 2004). Hereafter we will refer to this sonic point as the outer sonic point.…”

Section: Boundary Conditions and The Appropriate Integral Curvementioning

confidence: 99%

“…In order to select a proper integral curve we take a trial stagnation radius and then select T st from our first boundary condition, which requires the outer sonic point to be located at the star cluster surface (see Silich et al 2004;Tenorio-Tagle et al 2007). We then calculate the number density of the plasma at the stagnation radius from equation (13) and use these R st , T st , and n st as initial conditions to the backward integration from R st toward the star cluster center.…”

Section: Boundary Conditions and The Appropriate Integral Curvementioning

confidence: 99%

“…Second, it should account for radiative losses of energy from the hot thermal plasma. Third, the models should incorporate initial and boundary conditions as described by the star cluster wind theory (Chevalier & Clegg 1985;Cantó et al 2000;Silich et al 2004;Tenorio-Tagle et al 2007). …”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Spherically Symmetric Accretion onto a Black Hole at the Center of a Young Stellar Cluster

Silich

Tenorio-Tagle

Hueyotl-Zahuantitla

2008

Astrophysical Journal

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Here we present a self-consistent, bimodal stationary solution for spherically symmetric flows driven by young massive stellar clusters with a central supermassive black hole (SMBH ). We demonstrate that the hydrodynamic regime of the flow depends on the location of the cluster in the 3D (star cluster mechanical luminosityYBH massY star cluster radius) parameter space. We show that a threshold mechanical luminosity (L crit ) separates clusters that evolve in the BH-dominated regime from those whose internal structure is strongly affected by the radiative cooling. In the first case ( below the threshold energy) gravity of the BH separates the flow into two distinct zones: the inner accretion zone and the outer zone where the star cluster wind is formed. In the second case (above the critical luminosity), catastrophic cooling sets in inside the cluster. In this case the injected plasma becomes thermally unstable, which inhibits a complete stationary solution. We compared the calculated accretion rates and the BH luminosities with those predicted by the classic Bondi accretion theory and found that Bondi's theory is in good agreement with our results in the case of low-mass clusters. However, it substantially underestimates the accretion rates and BH luminosities if the star cluster mechanical luminosity L SC ! 0:1L crit .

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A Brief Galactic Winds and the Role Played by Massive Stars

Heckman¹,

Thompson²

2016

Handbook of Supernovae

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Winds Driven by Super Star Clusters: The Self‐Consistent Radiative Solution

Cited by 141 publications

References 24 publications

Gravitational and mass distribution effects on stationary superwinds

Gravitational and mass distribution effects on stationary superwinds

Spherically Symmetric Accretion onto a Black Hole at the Center of a Young Stellar Cluster

A Brief Galactic Winds and the Role Played by Massive Stars

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