Simulating Star Formation and Feedback in Galactic Disk Models

Tasker, Elizabeth J.; Bryan, Greg L.

doi:10.1086/500567

Cited by 120 publications

(170 citation statements)

References 52 publications

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“…Some authors report very efficient winds, even in the quite massive galaxies (Springel & Hernquist 2003;Tasker & Bryan 2006), while other authors obtained very low ejection efficiency, mainly in dwarf galaxies (Mac Low & Ferrara 1999). We believe that these differences arise partly from the different numerical techniques used, and partly from the different boundary conditions imposed around the galaxy.…”

Section: Introductionmentioning

confidence: 99%

“…In the recent literature, this same problem was addressed using smooth particle hydrodynamics (SPH) techniques reported by Springel & Hernquist (2003). Grid-based simulations were also performed, but using isolated, pre-formed rotating discs (Fujita et al 2004;Tasker & Bryan 2006). One of the key outcome of such numerical simulations is the fraction of the injected SNe energy which is transferred up to the large scale galactic wind and is truly available for feedback (Fujita et al 2004;Scannapieco et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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On the onset of galactic winds in quiescent star forming galaxies

Dubois¹,

Teyssier²

2007

A&A

281

367

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Context. The hierarchical model of galaxy formation, despite its many successes, still overpredicts the baryons fraction locked in galaxies as a condensed phase. The efficiency of supernovae feedback, proposed a long time ago as a possible solution for this socalled "overcooling" problem, is still under debate, mainly because modelling supernovae explosions within a turbulent interstellar medium, while capturing realistic large scale flows around the galaxy is a very demanding task. Aims. Our goal is to study the effect of supernovae feedback on a disc galaxy, taking into account the impact of infalling gas on both the star formation history and the corresponding outflow structure, the apparition of a supernovae-driven wind being highly sensitive to the halo mass, the galaxy spin and the star formation efficiency. Methods. We model our galaxies as cooling and collapsing NFW spheres. The dark matter component is modelled as a static external potential, while the baryon component is described by the Euler equations using the AMR code RAMSES. Metal-dependent cooling and supernovae-heating are also implemented using state-of-the-art recipes coming from cosmological simulations. We allow for three parameters to vary: the halo circular velocity, the spin parameter and the star formation efficiency. Results. We found that the ram pressure of infalling material is the key factor limiting the apparition of galactic winds. We obtain a very low feedback efficiency, with supernovae to wind energy conversion factor around one percent, so that only low circular velocity galaxies give rise to strong winds. For massive galaxies, we obtain a galactic fountain, for which we discuss the observational properties. Conclusions. We conclude that for quiescent isolated galaxies, galactic winds appear only in very low mass systems. Although this can quite efficiently enrich the IGM with metals, they do not carry away enough cold material to solve the overcooling problem.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

On the onset of galactic winds in quiescent star forming galaxies

Dubois¹,

Teyssier²

2007

A&A

281

367

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“…The low-density warm medium is distributed among a variety of densities and pressures, similar to our models. Wada & Norman (2007) perform global simulations of a SNe-driven ISM, but for similar reasons comparisons are difficult, as is the case for Slyz et al (2005), Korpi et al (1999), and Tasker & Bryan (2006). A similar code comparison such as the one presented here, but with SNe driven turbulence, would be very useful.…”

Section: Comparison With Previously Published Resultsmentioning

confidence: 99%

Multiphase ISM simulations: comparing NIRVANA and ZEUS

Piontek¹,

Gressel²,

Ziegler³

2009

A&A

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Aims. Our aim is to compare the ZEUS and NIRVANA MHD codes in their application to multi-phase ISM simulations. A contrast in density of about 100 between the warm and cold ISM phases is typical, and discontinuities such as these can be difficult to handle numerically. It is plausible that the details of implementing a particular numerical method could affect the results of the simulation, particularly with regard to the mass and volume fractions of the warm, unstable, and cold gas. This work takes a step towards quantifying to what extent this may occur. Methods. Using the NIRVANA code, we simulate a multi-phase ISM with turbulence driven by the magnetorotational instability. We make comparisons to our previously published ZEUS models and assess the impact of the numerical method on quantities such as the mass and volume fractions in the ISM phases, turbulent velocities, and probability distribution functions of density, temperature, pressure, and magnetic field strength. We also compare models with which turbulence is driven by an artificial forcing function. Results. For the models that include turbulence driven by the magnetorotational instability, we find differences in the mass fractions that are typically on the order of 10%. This comparison, however, is complicated by the result that the saturation level of the MRI is different between the two codes. This suggests that, at the same saturation level, we would expect to find larger differences in the mass fractions, and this is indeed what we have found for our artificially forced models. For these runs we find differences in the cold mass fraction of approximately 30%, which is significant.

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“…to reproduce gas structures in galaxy disks and galactic winds (e.g. undertaken by Tasker & Bryan (2006 with SF = 0.05 and 0.5). In addition, specific SN energy deposit SN × E SN /M * by them is fixed to 10 51 erg per 55 M of formed stars (1.8 × 10 49 erg M −1 by Dalla Vecchia & Schaye (2008)), but their results cannot ye tbe treated quantitatively, since they also mismatch with the Kennicutt relation.…”

Section: Supernova Parametrization In Numerical Modelsmentioning

confidence: 99%

The Supernova – ISM/Star-formation interplay

Hensler¹

2013

Proc. IAU

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Abstract. Supernovae are the most energetic stellar events and influence the interstellar medium by their gasdynamics and energetics. By this, both also affect the star formation positively and negatively. In this paper, we review the complexity of investigations aiming at understanding the interchange between supernova explosions with the star-forming molecular clouds. Commencing from analytical studies the paper advances to numerical models of supernova feedback from superbubble scales to galaxy structure. We also discuss parametrizations of star-formation and supernova-energy transfer efficiencies. Since evolutionary models from the interstellar medium to galaxies are numerous and are applying multiple recipes of these parameters, only a representative selection of studies can be discussed here.

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Simulating Star Formation and Feedback in Galactic Disk Models

Cited by 120 publications

References 52 publications

On the onset of galactic winds in quiescent star forming galaxies

On the onset of galactic winds in quiescent star forming galaxies

Multiphase ISM simulations: comparing NIRVANA and ZEUS

The Supernova – ISM/Star-formation interplay

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