Modelling the supernova-driven ISM in different environments

Gatto, Andrea; Walch, Stefanie; Low, Mordecai–Mark Mac; Naab, Thorsten; Girichidis, Philipp; Glover, Simon C. O.; Wünsch, Richard; Klessen, Ralf S.; Clark, Paul; Baczynski, Christian; Peters, Thomas; Ostriker, Jeremiah P.; Ibáñez-Mejía, Juan C.; Haid, S.

doi:10.1093/mnras/stv324

Cited by 153 publications

(146 citation statements)

References 120 publications

(140 reference statements)

Supporting

Mentioning

142

Contrasting

Unclassified

Order By: Relevance

“…These approximations give reasonable results for the gas in the disc, but the low-Mach outflowing gas is not treated correctly essentially because the hot phase produced by supernova explosions, which is largely responsible of gas expulsion, is absent from these simulations. We recall that the exact way supernova feedback is implemented has been found to have a drastic influence on the results (Hennebelle & Iffrig 2014;Gatto et al 2015). In particular if the supernovae are not sufficiently correlated with the dense gas, they do not exert any substantial influence on the star forming gas and this leads to very high SFR.…”

Section: Supernova Feedbackmentioning

confidence: 99%

“…Tasker & Bryan 2006;Dubois & Teyssier 2008;Bournaud et al 2010;Kim et al 2011;Dobbs et al 2011;Tasker 2011;Hopkins et al 2011;Renaud et al 2013), with a well-resolved interstellar medium (ISM) although the spatial resolution is continuously improving. To address this question, an alternative approach has been developed which consists of simulating a small portion of a galactic disc leading to a better spatial resolution (Korpi et al 1999;Slyz et al 2005;de Avillez & Breitschwerdt 2005;Joung & Mac Low 2006;Hill et al 2012;Kim et al 2011Kim et al , 2013Gent et al 2013;Hennebelle & Iffrig 2014;Gatto et al 2015) although at the expense of solving the large galactic scales. Clearly these two approaches are complementary and must be used in parallel.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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

Iffrig

Hennebelle

2017

A&A

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

Section: Supernova Feedbackmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Iffrig

Hennebelle

2017

A&A

View full text Add to dashboard Cite

show abstract

“…In our model, each SN releases an energy of ESN, which is typically injected in the form of thermal energy provided that the adiabatic phase of the SN remnant is resolved. If the density in the injection region is high, such that the Sedov-Taylor phase would be unresolved, we switch to a momentum input scheme (see Gatto et al 2015, for a detailed description of the SN model). The mass of the SN progenitor star is also added to the injection region.…”

Section: Stellar Wind Feedbackmentioning

confidence: 99%

The SILCC project – III. Regulation of star formation and outflows by stellar winds and supernovae

Gatto

Walch

Naab

et al. 2016

Mon. Not. R. Astron. Soc.

213

188

View full text Add to dashboard Cite

We study the impact of stellar winds and supernovae on the multi-phase interstellar medium using three-dimensional hydrodynamical simulations carried out with FLASH. The selected galactic disc region has a size of (500 pc) 2 × ±5 kpc and a gas surface density of 10 M pc −2 . The simulations include an external stellar potential and gas self-gravity, radiative cooling and diffuse heating, sink particles representing star clusters, stellar winds from these clusters which combine the winds from individual massive stars by following their evolution tracks, and subsequent supernova explosions. Dust and gas (self-)shielding is followed to compute the chemical state of the gas with a chemical network. We find that stellar winds can regulate star (cluster) formation. Since the winds suppress the accretion of fresh gas soon after the cluster has formed, they lead to clusters which have lower average masses (10 2 −10 4.3 M ) and form on shorter timescales (10 −3 −10 Myr). In particular we find an anti-correlation of cluster mass and accretion time scale. Without winds the star clusters easily grow to larger masses for ∼ 5 Myr until the first supernova explodes. Overall the most massive stars provide the most wind energy input, while objects beginning their evolution as B type stars contribute most of the supernova energy input. A significant outflow from the disk (mass loading 1 at 1 kpc) can be launched by thermal gas pressure if more than 50% of the volume near the disc mid-plane can be heated to T > 3 × 10 5 K. Stellar winds alone cannot create a hot volume-filling phase. The models which are in best agreement with observed star formation rates drive either no outflows or weak outflows.

show abstract

“…On the other hand, if a SN explodes in an environment dominated by tenuous gas, then the cooling is much less efficient, and a significant fraction of energy can be preserved (e.g. Li et al 2015;Gatto et al 2015;Simpson et al 2014;Walch et al 2015;Hennebelle & Iffrig 2014). One key factor to determine where SNe explode is the fact that a significant fraction of OB stars are "runaways", that is, having high velocities.…”

Section: Effects Of Several Physical Processesmentioning

confidence: 99%

Quantifying Supernovae-driven Multiphase Galactic Outflows

Li¹,

Bryan²,

Ostriker³

2017

ApJ

134

119

View full text Add to dashboard Cite

Galactic outflows are ubiquitously observed in star-forming disk galaxies and are critical for galaxy formation. Supernovae (SNe) play the key role in driving the outflows, but there is no consensus as to how much energy, mass and metal they can launch out of the disk. We perform 3D, high-resolution hydrodynamic simulations to study SNe-driven outflows from stratified media. Assuming SN rate scales with gas surface density Σ gas as in the Kennicutt-Schmidt (KS) relation, we find the mass loading factor, η m , defined as the mass outflow flux divided by the star formation surface density, decreases with increasing Σ gas as η m ∝ Σ −0.61 gas . Approximately Σ gas 50M / pc 2 marks when η m 1. About 10-50% of the energy and 40-80% of the metals produced by SNe end up in the outflows. The tenuous hot phase (T > 3×10 5 K), which fills 60-80% of the volume at mid-plane, carries the majority of the energy and metals in outflows. We discuss how various physical processes, including vertical distribution of SNe, photoelectric heating, external gravitational field and SN rate, affect the loading efficiencies. The relative scale height of gas and SNe is a very important factor in determining the loading efficiencies.

show abstract

Modelling the supernova-driven ISM in different environments

Cited by 153 publications

References 120 publications

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

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

The SILCC project – III. Regulation of star formation and outflows by stellar winds and supernovae

Quantifying Supernovae-driven Multiphase Galactic Outflows

Contact Info

Product

Resources

About