Feedback in Clouds II: UV photoionization and the first supernova in a massive cloud

Geen, Sam; Hennebelle, P.; Tremblin, Pascal; Rosdahl, Joakim

doi:10.1093/mnras/stw2235

Cited by 98 publications

(97 citation statements)

References 83 publications

(123 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The shell formation time terminates the radial momentum generation phase (see Haid et al 2016 for a detailed discussion of the momentum generating phases) and the remnant transits to the momentum conserving snow plough phase. In Figure 7 we show an updated version of Figure 4 of Naab & Ostriker (2017) with a comparison of the momentum gain for different ambient densities to previous estimates by Cioffi et al (1988); Martizzi et al (2015); Iffrig & Hennebelle (2015); Li et al (2017); Kim & Ostriker (2015); Walch et al (2015); Geen et al (2016). Our results agree well in particular with Kim & Ostriker (2015) and show a momentum boost compared to the assumed initial SN momentum of p 0 = 14181 M km s −1 from a factor ∼ 10 at n = 100 cm −3 to a factor ∼ 50 at n = 0.001 cm −3 .…”

Section: Environmental Dependencementioning

confidence: 99%

Hot phase generation by supernovae in ISM simulations: resolution, chemistry, and thermal conduction

Steinwandel

Moster

Naab

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Supernovae (SN) generate hot gas in the interstellar medium (ISM), help setting the ISM structure and support the driving of outflows. It is important to resolve the hot gas generation for galaxy formation simulations at solar mass and sub-parsec resolution which realise individual supernova (SN) explosions with ambient densities varying by several orders of magnitude in a realistic multi-phase ISM. We test resolution requirements by simulating SN blast waves at three metallicities (Z = 0.01, 0.1 and 1Z ), six densities and their respective equilibrium chemical compositions (n = 0.001 cm −3 -100 cm −3 ), and four mass resolutions (0.1 -100 M ). We include non-equilibrium cooling and chemistry, a homogenous interstellar radiation field, and shielding with a modern pressure-energy smoothed particle hydrodynamics (SPH) method including isotropic thermal conduction and a meshless-finite-mass (MFM) solver. We find stronger resolution requirements for chemistry and hot phase generation than for momentum generation. While at 10 M the radial momenta at the end of the Sedov phase start converging, the hot phase generation and chemistry require higher resolutions to represent the neutral to ionised hydrogen fraction at the end of the Sedov phase correctly. Thermal conduction typically reduces the hot phase by 0.2 dex and has little impact on the chemical composition. In general, our 1, and 0.1 M results agree well with previous numerical and analytic estimates. We conclude that for the thermal energy injection SN model presented here resolutions higher than 10 M are required to model the chemistry, momentum and hot phase generation in a multi-phase ISM.

show abstract

Section: Environmental Dependencementioning

confidence: 99%

Hot phase generation by supernovae in ISM simulations: resolution, chemistry, and thermal conduction

Steinwandel

Moster

Naab

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…For each simulation we estimate the total hydrogenionising photon emission rate at a given time as S cl (m cl ) = 8.96 × 10 46 s −1 (m cl /M ) (see Geen et al 2017), where m cl is the total mass of the sink particles. This is calculated by Monte Carlo sampling a stellar population as described in Geen et al (2016) (See Sec. B).…”

Section: Feedback and Properties Of Uv Sourcementioning

confidence: 99%

Simulating star clusters across cosmic time – I. Initial mass function, star formation rates, and efficiencies

Ricotti

Geen

2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present radiation-magneto-hydrodynamic simulations of star formation in selfgravitating, turbulent molecular clouds, modeling the formation of individual massive stars, including their UV radiation feedback. The set of simulations have cloud masses between m gas = 10 3 M to 3 × 10 5 M and gas densities typical of clouds in the local universe (n gas ∼ 1.8 × 10 2 cm −3 ) and 10× and 100× denser, expected to exist in high-redshift galaxies. The main results are: i) The observed Salpeter power-law slope and normalisation of the stellar initial mass function at the high-mass end can be reproduced if we assume that each star-forming gas clump (sink particle) fragments into stars producing on average a maximum stellar mass about 40% of the mass of the sink particle, while the remaining 60% is distributed into smaller mass stars. Assuming that the sinks fragment according to a power-law mass function flatter than Salpeter, with log-slope 0.8, satisfy this empirical prescription. ii) The star formation law that best describes our set of simulation is dρ * /dt ∝ ρ 1.5 gas if n gas < n cri ≈ 10 3 cm −3 , and dρ * /dt ∝ ρ 2.5 gas otherwise. The duration of the star formation episode is roughly 6 cloud's sound crossing times (with c s = 10 km/s). iii) The total star formation efficiency in the cloud is f * = 2%(m gas /10 4 M ) 0.4 (1 + n gas /n cri ) 0.91 , for gas at solar metallicity, while for metallicity Z < 0.1 Z , based on our limited sample, f * is reduced by a factor of ∼ 5. iv) The most compact and massive clouds appear to form globular cluster progenitors, in the sense that star clusters remain gravitationally bound after the gas has been expelled.

show abstract

“…Since treating precisely the dense gas and the supernova correlation implies resolving not only the star formation well but also following the detailed star trajectories, this constitutes a very difficult task, that renders prescriptions like the one we are using unavoidable. More generally, other sources of feedback such as HII radiation and stellar winds should be considered as well (Walch et al 2012;Dale et al 2013Dale et al , 2014Geen et al 2015Geen et al , 2016.…”

Section: Supernova Feedbackmentioning

confidence: 99%

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

Iffrig

Hennebelle

2017

A&A

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Feedback in Clouds II: UV photoionization and the first supernova in a massive cloud

Cited by 98 publications

References 83 publications

Hot phase generation by supernovae in ISM simulations: resolution, chemistry, and thermal conduction

Hot phase generation by supernovae in ISM simulations: resolution, chemistry, and thermal conduction

Simulating star clusters across cosmic time – I. Initial mass function, star formation rates, and efficiencies

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

Contact Info

Product

Resources

About