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

Martizzi, Davidé; Fielding, Drummond B.; Faucher-Giguère, Claude André; Quataert, Eliot

doi:10.1093/mnras/stw745

Cited by 126 publications

(143 citation statements)

References 70 publications

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“…Overall, we find a very good correlation between η E and the ISM condition: η E 0.08 when ISM is "breakout"; η E 0.01 when ISM is "non-breakout"; η E ∼ 0.01-0.08 when ISM is "partial-breakout". We note that "partial-breakout", in reality, can either be due to the final, quasi-steady ISM state falling into the criterion (Martizzi et al 2016), or the ISM transitioning/cycling between the non-breakout and the breakout states (Kim & Ostriker 2018).…”

Section: Sfrmentioning

confidence: 99%

Simple Yet Powerful: Hot Galactic Outflows Driven by Supernovae

Bryan

2020

ApJL

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Supernovae (SNe) drive multiphase galactic outflows, impacting galaxy formation; however, cosmological simulations mostly use ad hoc feedback models for outflows, making outflow-related predictions from first principles problematic. Recent small-box simulations resolve individual SNe remnants in the interstellar medium (ISM), naturally driving outflows and permitting a determination of the wind loading factors of energy η E , mass η m , and metals η Z . In this Letter, we compile small-box results, and find consensus that the hot outflows are much more powerful than the cool outflows: (i) their energy flux is 2-20 times greater, and (ii) their specific energy e s,h is 10-1000 times higher. Moreover, the properties of hot outflows are remarkably simple: e s,h ∝ η E,h /η m,h is almost invariant over four orders of magnitude of star formation surface density. Also, we find tentatively that η E,h /η Z,h ∼ 0.5. If corroborated by more simulation data, these correlations reduce the three hot phase loading factors into one. Finally, this one parameter is closely related to whether the ISM has a "breakout" condition. The narrow range of e s,h indicates that hot outflows cannot escape dark matter halos with log M halo [M ] 12. This mass is also where the galaxy mass-metallicity relation reaches its plateau, implying a deep connection between hot outflows and galaxy formation. We argue that hot outflows should be included explicitly in cosmological simulations and (semi-)analytic modeling of galaxy formation.

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Section: Sfrmentioning

confidence: 99%

Simple Yet Powerful: Hot Galactic Outflows Driven by Supernovae

Bryan

2020

ApJL

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“…For our model we account for the entire galactic disc, although this imposes constraints on the spatial resolution we can afford. As was pointed out by Martizzi et al (2016), not accounting for the global geometry of the disc, as is the case for ISM patches, leads to unreliable wind properties due to incorrect treatment of the gravitational potential and the disc rotation.…”

Section: Comparison To Other Workmentioning

confidence: 99%

How runaway stars boost galactic outflows

Andersson

Agertz

2020

Monthly Notices of the Royal Astronomical Society

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Roughly ten per cent of OB stars are kicked out of their natal clusters before ending their life as supernovae. These so called runaway stars can travel hundreds of parsecs into the low-density interstellar medium, where momentum and energy from stellar feedback is efficiently deposited. In this work we explore how this mechanism affects large scale properties of the galaxy, such as outflows. To do so we use a new model which treats OB stars and their associated feedback processes on a star-by-star basis. With this model we compare two hydrodynamical simulations of Milky Way-like galaxies, one where we include runaways, and one where we ignore them. Including runaway stars leads to twice as many supernovae explosions in regions with gas densities ranging from 10 −5 cm −3 to 10 −3 cm −3 . This results in more efficient heating of the inter-arm regions, and drives strong galactic winds with mass loading factors boosted by up to one order of magnitude. These outflows produce a more massive and extended multi-phase circumgalactic medium, as well as a population of dense clouds in the halo. Conversely, since less energy and momentum is released in the dense star forming regions, the cold phase of the interstellar medium is less disturbed by feedback effects.

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“…Several decades of research in this area have identified stellar feedback as one of the leading physical processes to explain this inefficiency in L * galaxies and below (e.g. Stinson et al 2006;Sales et al 2010;Ostriker & Shetty 2011;Hopkins et al 2014a;Kimm & Cen 2014;Marinacci et al 2014;Vogelsberger et al 2014;Murante et al 2015;Wang et al 2015;Schaye et al 2015;Martizzi et al 2016;Li et al 2017;. Resolving the multiphase structure of the ISM and a detailed modelling of stellar feedback are therefore key targets in modern studies of galaxy formation.…”

Section: Introductionmentioning

confidence: 99%

Simulating the interstellar medium and stellar feedback on a moving mesh: implementation and isolated galaxies

Marinacci

Sales

Vogelsberger

et al. 2019

Monthly Notices of the Royal Astronomical Society

115

131

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We introduce the Stars and MUltiphase Gas in GaLaxiEs -SMUGGLE model, an explicit and comprehensive stellar feedback model for the moving-mesh code AREPO. This novel sub-resolution model resolves the multiphase gas structure of the interstellar medium and self-consistently generates gaseous outflows. The model implements crucial aspects of stellar feedback including photoionization, radiation pressure, energy and momentum injection from stellar winds and from supernovae. We explore this model in high-resolution isolated simulations of Milky Way-like disc galaxies. Stellar feedback regulates star formation to the observed level and naturally captures the establishment of a Kennicutt-Schmidt relation. This result is achieved independent of the numerical mass and spatial resolution of the simulations. Gaseous outflows are generated with average mass loading factors of the order of unity. Strong outflow activity is correlated with peaks in the star formation history of the galaxy with evidence that most of the ejected gas eventually rains down onto the disc in a galactic fountain flow that sustains late-time star formation. Finally, the interstellar gas in the galaxy shows a distinct multiphase distribution with a coexistence of cold, warm and hot phases.

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

Cited by 126 publications

References 70 publications

Simple Yet Powerful: Hot Galactic Outflows Driven by Supernovae

Simple Yet Powerful: Hot Galactic Outflows Driven by Supernovae

How runaway stars boost galactic outflows

Simulating the interstellar medium and stellar feedback on a moving mesh: implementation and isolated galaxies

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