Vertical Equilibrium, Energetics, and Star Formation Rates in Magnetized Galactic Disks Regulated by Momentum Feedback From Supernovae

Kim, Chang-Goo; Ostriker, Eve C.

doi:10.1088/0004-637x/815/1/67

Cited by 120 publications

(148 citation statements)

References 91 publications

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“…We continue to adopt the local box approximation, focusing on ∼ 1 kpc 3 patches of galactic discs. Several previous SN feedback studies have included vertical stratification in local boxes (Dib et al 2006;Joung & Mac Low 2006;Joung et al 2009;Creasey et al 2013;Kim et al 2013;Kim & Ostriker 2015b;. Our analysis complements various subsets of these previous studies in different ways.…”

Section: Introductionmentioning

confidence: 55%

“…In particular, we implemented the subgrid model derived in that study to capture the momentum injection and thermal energy of individual SNe when the Sedov-Taylor phase of the remnants is not well resolved. A number of other papers have reported closely related local simulations of SN feedback in vertically stratified media, with varying degrees of complexity (e.g., Dib et al 2006;Joung & Mac Low 2006;Joung et al 2009;Shetty & Ostriker 2012;Creasey et al 2013;Hennebelle & Iffrig 2014;Kim & Ostriker 2015b;. Our study adds to this body of work by providing a detailed analysis of the turbulence and wind properties as a function of gas surface density and SN seeding scheme, as well as an analysis of the limitations of local Cartesian box simulations for predicting the properties of galactic winds.…”

Section: Discussionmentioning

confidence: 78%

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Supernova feedback in a local vertically stratified medium: interstellar turbulence and galactic winds

Martizzi

Fielding

Faucher-Giguère

et al. 2016

Mon. Not. R. Astron. Soc.

126

134

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We use local Cartesian simulations with a vertical gravitational potential to study how supernova (SN) feedback in stratified galactic discs drives turbulence and launches galactic winds. Our analysis includes three disc models with gas surface densities ranging from Milky Way-like galaxies to gas-rich ultra-luminous infrared galaxies (ULIRGs), and two different SN driving schemes (random and correlated with local gas density). In order to isolate the physics of SN feedback, we do not include additional feedback processes. We find that, in these local box calculations, SN feedback excites relatively low mass-weighted gas turbulent velocity dispersions ≈ 3 − 7 km s −1 and low wind mass loading factors η 1 in all the cases we study. The low turbulent velocities and wind mass loading factors predicted by our local box calculations are significantly below those suggested by observations of gas-rich and rapidly star-forming galaxies; they are also in tension with global simulations of disc galaxies regulated by stellar feedback. Using a combination of numerical tests and analytic arguments, we argue that local Cartesian boxes cannot predict the properties of galactic winds because they do not capture the correct global geometry and gravitational potential of galaxies. The wind mass loading factors are in fact not well-defined in local simulations because they decline significantly with increasing box height. More physically realistic calculations (e.g., including a global galactic potential and disc rotation) will likely be needed to fully understand disc turbulence and galactic outflows, even for the idealized case of feedback by SNe alone.

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Section: Introductionmentioning

confidence: 55%

Section: Discussionmentioning

confidence: 78%

Supernova feedback in a local vertically stratified medium: interstellar turbulence and galactic winds

Martizzi

Fielding

Faucher-Giguère

et al. 2016

Mon. Not. R. Astron. Soc.

126

134

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“…All simulations, except B0, have been run up to 80 Myr. Apart from the weak feedback cases, our simulation are similar to the ones performed by Kim & Ostriker (2015b) except that we did not treat the shear and we have higher numerical resolution.…”

Section: Runs Performedmentioning

confidence: 95%

Structure distribution and turbulence in self-consistently supernova-driven ISM of multiphase magnetized galactic discs

Iffrig

Hennebelle

2017

A&A

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Context. Galaxy evolution and star formation are two multi-scale problems tightly linked to each other. Aims. We aim to describe simultaneously the large-scale evolution widely induced by the feedback processes and the details of the gas dynamics that controls the star formation process through gravitational collapse. This is a necessary step in understanding the interstellar cycle, which triggers galaxy evolution. Methods. We performed a set of three-dimensional high-resolution numerical simulations of a turbulent, self-gravitating and magnetized interstellar medium within a 1 kpc stratified box with supernova feedback correlated with star-forming regions. In particular, we focussed on the role played by the magnetic field and the feedback on the galactic vertical structure, the star formation rate (SFR) and the flow dynamics. For this purpose we have varied their respective intensities. We extracted properties of the dense clouds arising from the turbulent motions and compute power spectra of various quantities. Results. Using a distribution of supernovae sufficiently correlated with the dense gas, we find that supernova explosions can reproduce the observed SFR, particularly if the magnetic field is on the order of a few µG. The vertical structure, which results from a dynamical and an energy equilibrium is well reproduced by a simple analytical model, which allows us to roughly estimate the efficiency of the supernovae in driving the turbulence in the disc to be rather low, of the order of 1.5%. Strong magnetic fields may help to increase this efficiency by a factor of between two and three. To characterize the flow we compute the power spectra of various quantities in 3D but also in 2D in order to account for the stratification of the galactic disc. We find that within our setup, the compressive modes tend to dominate in the equatorial plane, while at about one scale height above it, solenoidal modes become dominant. We measured the angle between the magnetic and velocity fields and we conclude that they tend to be well aligned particularly at high magnetization and lower feedback. Finally, the dense structures present scaling relations that are reminiscent of the observational ones. The virial parameter is typically larger than 10 and shows a large spread of masses below 1000 M . For masses larger than 10 4 M , its value tends to a few. Conclusions. Using a relatively simple scheme for the supernova feedback, which is self-consistently proportional to the SFR and spatially correlated to the star formation process, we reproduce a stratified galactic disc that presents reasonable scale height, SFR as well as a cloud distribution with characteristics close to the observed ones.

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“…) that follows space-time correlation of supernovae (SNe) with dense and diffuse gas realistically, resolves all thermal phases of the ISM (the hot phase was missing previously), and fully captures the circulation of the galactic fountain. In particular, the amount of radial momentum injection per SN (p * ) is self-consistently determined by numerically resolving supernova remnant expansion prior to the onset of cooling (Kim & Ostriker 2015) in contrast to the previous simulations where it was fixed to p * = 3 × 10 5 M ⊙ km s −1 . If we assume f H2,diff = 0 we find a mean α of 2.6 (red dotted line), which is about ∼ 30% lower than the α values resulting from the simulations.…”

Section: Dependence On Metallicitymentioning

confidence: 99%

Thermal Pressure in the Cold Neutral Medium of Nearby Galaxies

Herrera-Camus

Bolatto

Wolfire

et al. 2017

ApJ

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Dynamic and thermal processes regulate the structure of the multi-phase interstellar medium (ISM), and ultimately establish how galaxies evolve through star formation. Thus, to constrain ISM models and better understand the interplay of these processes, it is of great interest to measure the thermal pressure (P th ) of the diffuse, neutral gas. By combining [C II] 158 µm, HI, and CO data from 31 galaxies selected from the Herschel KINGFISH sample, we have measured thermal pressures in 534 predominantly atomic regions with typical sizes of ∼1 kiloparsec. We find a distribution of thermal pressures in the P th /k ∼ 10 3 − 10 5 K cm −3 range. For a sub-sample of regions with conditions similar to those of the diffuse, neutral gas in the Galactic plane, we find thermal pressures that follow a log-normal distribution with a median value of P th /k ≈ 3600 K cm −3 . These results are consistent with thermal pressure measurements using other observational methods. We find that P th increases with radiation field strength and star formation activity, as expected from the close link between the heating of the gas and the star formation rate. Our thermal pressure measurements fall in the regime where a two-phase ISM with cold and warm neutral medium could exist in pressure equilibrium. Finally, we find that the midplane thermal pressure of the diffuse gas is about ∼ 30% of the vertical weight of the overlying ISM, consistent with results from hydrodynamical simulations of self-regulated star formation in galactic disks.

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Vertical Equilibrium, Energetics, and Star Formation Rates in Magnetized Galactic Disks Regulated by Momentum Feedback From Supernovae

Cited by 120 publications

References 91 publications

Supernova feedback in a local vertically stratified medium: interstellar turbulence and galactic winds

Supernova feedback in a local vertically stratified medium: interstellar turbulence and galactic winds

Structure distribution and turbulence in self-consistently supernova-driven ISM of multiphase magnetized galactic discs

Thermal Pressure in the Cold Neutral Medium of Nearby Galaxies

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