Cosmological galaxy evolution with superbubble feedback – I. Realistic galaxies with moderate feedback

Keller, Ben; Wadsley, James; Couchman, H. M. P.

doi:10.1093/mnras/stv1789

Cited by 74 publications

(99 citation statements)

References 75 publications

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“…Keller et al (2014) describe such a parameter-free, resolution-independent SN feedback model. Similarly to early stellar feedback models, this model is able to reduce star formation before z = 2 and to produce a Milky-Way-mass galaxy with low bulge-to-total mass ratio (Keller et al 2015).…”

Section: Discussionmentioning

confidence: 91%

“…This analysis enables us to independently study inflows, outflows, and recycling as a function of galaxy mass, which allows a deeper investigation into the underlying physical processes that govern the baryon cycle. The details of baryon cycling presented here do depend on our methodology for driving outflows and may vary for different choices of physical models (see, e.g., Keller et al 2015;Muratov et al 2015). Nonetheless, our results are of particular interest since our outflow driving model yields a viable match to numerous key observational constraints, as we will show.…”

Section: The Analysis Of Outflows Presented Herementioning

confidence: 82%

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In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Christensen

Davé

Governato

et al. 2016

ApJ

212

250

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We examine the scalings of galactic outflows with halo mass across a suite of 20 high-resolution cosmological zoom galaxy simulations covering halo masses in the range - . These simulations self-consistently generate outflows from the available supernova energy in a manner that successfully reproduces key galaxy observables, including the stellar mass-halo mass, Tully-Fisher, and mass-metallicity relations. We quantify the importance of ejective feedback to setting the stellar mass relative to the efficiency of gas accretion and star formation. Ejective feedback is increasingly important as galaxy mass decreases; we find an effective mass loading factor that scales asv circ 2.2 , with an amplitude and shape that are invariant with redshift. These scalings are consistent with analytic models for energy-driven wind, based solely on the halo potential. Recycling is common: about half of the outflow mass across all galaxy masses is later reaccreted. The recycling timescale is typically ∼1 Gyr, virtually independent of halo mass. Recycled material is reaccreted farther out in the disk and with typically ∼2-3 times more angular momentum. These results elucidate and quantify how the baryon cycle plausibly regulates star formation and alters the angular momentum distribution of disk material across the halo mass range where most cosmic star formation occurs.

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Section: Discussionmentioning

confidence: 91%

Section: The Analysis Of Outflows Presented Herementioning

confidence: 82%

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Christensen

Davé

Governato

et al. 2016

ApJ

212

250

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“…There is a factor of several lower star formation after the initial burst in superbubble. This difference reflects the ability of superbubble to match naturally the stellar mass to halo mass relation at all redshifts in cosmological simulations (Keller et al 2015).…”

Section: Resultsmentioning

confidence: 98%

Clumpy Disks as a Testbed for Feedback-Regulated Galaxy Formation

Mayer

Tamburello

Lupi

et al. 2016

ApJL

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We study the dependence of fragmentation in massive gas-rich galaxy disks at z > 1 on feedback model and hydrodynamical method, employing the GASOLINE2 SPH code and the lagrangian meshless code GIZMO in finite mass mode. We compare non-cosmological galaxy disk runs with standard blastwave supernovae (SN)feedback, which introduces delayed cooling in order to drive winds, and runs with the new superbubble SN feedback, which produces winds naturally by modelling the detailed physics of SN-driven bubbles and leads to efficient self-regulation of star formation. We find that, with blastwave feedback, massive star forming clumps form in comparable number and with very similar masses in GASOLINE2 and GIZMO. The typical masses are in the range 10 7 − 10 8 M ⊙ , lower than in most previous works, while giant clumps with masses above 10 9 M ⊙ are exceedingly rare. With superbubble feedback, instead, massive bound star forming clumps do not form because galaxies never undergo a phase of violent disk instability. Only sporadic, unbound star forming overdensities lasting only a few tens of Myr can arise that are triggered by perturbations of massive satellite companions. We conclude that there is a severe tension between explaining massive star forming clumps observed at z > 1 primarily as the result of disk fragmentation driven by gravitational instability and the prevailing view of feedback-regulated galaxy formation. The link between disk stability and star formation efficiency should thus be regarded as a key testing ground for galaxy formation theory.

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“…All of these problems point towards a single potential solution: galaxies not only accrete gas, they eject it as well. Outflows driven by stellar feedback (Larson 1974;Keller et al 2015), active galactic nuclei (AGN) (Di Matteo et al 2005;Keller et al 2016), radiation (Murray et al 2011), or cosmic rays (Ipavich 1975) can all act to remove gas from the disc of a galaxy, dropping the baryon fraction, starving the star formation process, and polluting the CGM with metals and cold, entrained gas. How these outflows are launched, and the trajectory they take through the galactic corona is one of the most important unsolved problems in modern galaxy formation theory.…”

Section: Introductionmentioning

confidence: 99%

Entropy-driven winds: Outflows and fountains lifted gently by buoyancy

Keller

Kruijssen

Wadsley

2020

Monthly Notices of the Royal Astronomical Society

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We present a new theoretical framework for using entropy to understand how outflows driven by supernovae are launched from disc galaxies: via continuous, buoyant acceleration through the circumgalactic medium (CGM). When young star clusters detonate supernovae in the interstellar medium (ISM) of a galaxy, they generate hot, diffuse bubbles that push on the surrounding ISM and evaporate that ISM into their interiors. As these bubbles reach the scale height of the ISM, they break out of the disc, rising into the CGM. Once these bubbles break out, if they have sufficiently high entropy, they will feel an upward acceleration, owing to a local buoyant force. This upward force will accelerate these bubbles, driving them to high galactocentric radii, keeping them in the CGM for > Gyr, even if their initial velocity is much lower than the local escape velocity. We derive an equation of motion for these entropy-driven winds that connects the ISM properties, halo mass, and CGM profile of galaxies to the ultimate evolution of feedback-driven winds. We explore the parameter space of these equations, and show how this novel mechanism can explain both self-consistent simulations of star formation and galactic outflows as well as the new wealth of observations of CGM kinematics. We show that these entropy-driven winds can produce long wind recycling times, while still carrying a significant amount of mass. Comparisons to simulations and observations show entropy-driven winds convincingly explain the kinematics of galactic outflows.

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Cosmological galaxy evolution with superbubble feedback – I. Realistic galaxies with moderate feedback

Cited by 74 publications

References 75 publications

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Clumpy Disks as a Testbed for Feedback-Regulated Galaxy Formation

Entropy-driven winds: Outflows and fountains lifted gently by buoyancy

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