Turbulent Dissipation in the Interstellar Medium: The Coexistence of Forced and Decaying Regimes and Implications for Galaxy Formation and Evolution

Avila-Reese, Vladimir; Vázquez‐Semadeni, Enrique

doi:10.1086/320944

Cited by 34 publications

(15 citation statements)

References 60 publications

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“…An alternative to the present modelling is to consider the ISM as turbulent. As shown by Avila‐Reese & Vazquez‐Semadeni (2001), the ISM can be considered as a globally turbulent medium, with turbulence forced in specific places (the star‐forming regions) and propagating throughout the volume. The ‘diffusion’ velocity of turbulence is connected to the time‐scale of decay of turbulence.…”

Section: Discussionmentioning

confidence: 99%

“…This picture is challenged by the results of many simulation programs, aimed at the numerical modelling of the ISM (see, for example, Mac Low et al 1998; Ostriker, Gammie & Stone 1999; Avila‐Reese & Vazquez‐Semadeni 2001; Kritsuk & Norman 2002; see Mac Low 2002 and Vazquez‐Semadeni 2002 for reviews). In this context, the ISM is dominated by compressible, supersonic, MHD turbulence.…”

Section: Introductionmentioning

confidence: 99%

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Physical regimes for feedback in galaxy formation

Monaco

2004

Monthly Notices of the Royal Astronomical Society

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We present a new (semi-)analytic model for feedback in galaxy formation. The ISM is modeled as a two-phase medium in pressure equilibrium. The remnants of exploding type II SNe percolate into super-bubbles (SBs) that sweep the ISM, heating the hot phase (if the SB is adiabatic) or cooling it (in the snowplow stage, when the interior gas of the SB has cooled). The resulting feedback regimes occur in well-defined regions of the space defined by vertical scale-length and surface density of the structure. When SBs blow out in the adiabatic regime, the efficiency of SNe in heating the ISM is ~5 per cent, with \~80 per cent of the energy budget injected into the external halo, and the outcoming ISM is self-regulated to a state similar to that found in the Milky Way. Feedback is most efficient when SBs are pressure-confined in the adiabatic regime. In some significant regions of the parameter space confinement takes place in the snowplow stage; then the hot phase has a lower temperature and star formation is quicker. In some critical cases, the hot phase is strongly depleted and the cold phase percolates the whole volume, giving rise to a sudden burst of star formation. Strong galactic winds are predicted to happen only in critical cases. This model provides a starting point for constructing a realistic grid of feedback solutions to be used in galaxy formation codes. The predictive power of this model extends to many properties of the ISM, so that most parameters can be constrained by reproducing the main properties of the Milky Way. (Abridged)Comment: 27 pages, 10 postscript figures included, uses mn2e (included). In press on MNRA

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Physical regimes for feedback in galaxy formation

Monaco

2004

Monthly Notices of the Royal Astronomical Society

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“…A major discovery of simulations is that supersonic MHD turbulence decays in roughly a crossing time (based on the rms turbulent velocity) regardless of magnetic effects and the discreteness of energy injection (Mac Low et al 1998;Stone, Ostriker & Gammie 1998;Mac Low 1999;Avila-Reese & Vázquez-Semadeni 2001;Ostriker et al 2001). Decay is faster with cooling (Kritsuk & Norman 2002b, Pavlovski et al 2002 because the average Mach number is larger.…”

Section: Decay Of Supersonic Mhd Turbulencementioning

confidence: 99%

Interstellar Turbulence I: Observations and Processes

Elmegreen

Scalo

2004

Annu. Rev. Astron. Astrophys.

1,115

983

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Turbulence affects the structure and motions of nearly all temperature and density regimes in the interstellar gas. This two-part review summarizes the observations, theory, and simulations of interstellar turbulence and their implications for many fields of astrophysics. The first part begins with diagnostics for turbulence that have been applied to the cool interstellar medium, and highlights their main results. The energy sources for interstellar turbulence are then summarized along with numerical estimates for their power input. Supernovae and superbubbles dominate the total power, but many other sources spanning a large range of scales, from swing amplified gravitational instabilities to cosmic ray streaming, all contribute in some way. Turbulence theory is considered in detail, including the basic fluid equations, solenoidal and compressible modes, global inviscid quadratic invariants, scaling arguments for the power spectrum, phenomenological models for the scaling of higher order structure functions, the direction and locality of energy transfer and cascade, velocity probability distributions, and turbulent pressure. We emphasize expected differences between incompressible and compressible turbulence. Theories of magnetic turbulence on scales smaller than the collision mean free path are included, as are theories of magnetohydrodynamic turbulence and their various proposals for power spectra. Numerical simulations of interstellar turbulence are reviewed. Models have reproduced the basic features of the observed scaling relations, predicted fast decay rates for supersonic MHD turbulence, and derived probability distribution functions for density. Thermal instabilities and thermal phases have a new interpretation in a supersonically turbulent medium. Large-scale models with various combinations of self-gravity, magnetic fields, supernovae, and -2 -star formation are beginning to resemble the observed interstellar medium in morphology and statistical properties. The role of self-gravity in turbulent gas evolution is clarified, leading to new paradigms for the formation of star clusters, the stellar mass function, the origin of stellar rotation and binary stars, and the effects of magnetic fields. The review ends with a reflection on the progress that has been made in our understanding of the interstellar medium, and offers a list of outstanding problems.

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“…We will use γ in = σ z /v w . For the turbulence decay, several numerical studies have demonstrated that supersonic turbulence dissipates rapidly, in a timescale roughly equivalent to the crossing time for the driving scale at the turbulence velocity (e.g., Mac Low 1999;Stone et al 1999;Avila-Reese & Vázquez-Semadeni 2001). The latter authors have found values of t d ≈ 15 − 20 Myr for ISM properties typical of the MW.…”

Section: 5mentioning

confidence: 99%

Cosmological Simulations of Milky Way-Sized Galaxies

Colín

Avila-Reese

Roca-Fàbrega

et al. 2016

ApJ

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We introduce a new set of eight Milky Way-sized cosmological simulations performed using the AMR code ART + Hydrodynamics in a ΛCDM cosmology. The set of zoom-in simulations covers present-day virial masses that range from 8.3 × 10 11 M ⊙ to 1.56 × 10 12 M ⊙ and is carried out with our simple but effective deterministic star formation (SF) and "explosive" stellar feedback prescriptions. The work is focused on showing the goodness of the simulated set of "field" Milky Way-sized galaxies. To this end, we compare some of the predicted physical quantities with the corresponding observed ones. Our results are as follows. (a) In agreement with some previous works, we found circular velocity curves that are flat or slightly peaked. (b) All simulated galaxies with a significant disk component are consistent with the observed Tully-Fisher, radius-mass, and cold gas-stellar mass correlations of latetype galaxies. (c) The disk-dominated galaxies have stellar specific angular momenta in agreement with those of late-type galaxies, with values around 10 3 km/s/kpc. (d) The SF rates at z = 0 of all runs but one are comparable to those estimated for the star-forming galaxies. (e) The two most spheroid-dominated galaxies formed in halos with late active merger histories and late bursts of SF, but the other run that ends also as dominated by an spheroid, never had major mergers. (f) The simulated galaxies lie in the semi-empirical stellar-to-halo mass correlation of local central galaxies, and those that end up as disk dominated, evolve mostly along the low-mass branch of this correlation. Moreover, the baryonic and stellar mass growth histories of these galaxies are proportional to their halo mass growth histories since the last 6.5-10 Gyr. (g) Within the virial radii of the simulations, ≈ 25 − 50% of the baryons are missed; the amount of gas in the halo is similar to the one in stars in the galaxy, and most of this gas is in the warm-hot phase. (h) The z ∼ 0 vertical gas velocity dispersion profiles, σ z (r), are nearly flat and can be mostly explained by the kinetic energy injected by stars. The average values of σ z increase at higher redshifts, following roughly the shape of the SF history.

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Turbulent Dissipation in the Interstellar Medium: The Coexistence of Forced and Decaying Regimes and Implications for Galaxy Formation and Evolution

Cited by 34 publications

References 60 publications

Physical regimes for feedback in galaxy formation

Physical regimes for feedback in galaxy formation

Interstellar Turbulence I: Observations and Processes

Cosmological Simulations of Milky Way-Sized Galaxies

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