The dynamical destruction of shocked gas clouds

Nittmann, J.; Falle, S. A. E. G.; Gaskell, P. H.

doi:10.1093/mnras/201.4.833

Cited by 80 publications

(41 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For strong shocks, the cloud crushing time depends on the density contrast between the cloud and the ambient medium, the size of the cloud, and the speed of the shock. Earlier under-resolved numerical work came to similar conclusions (Nittmann et al 1982;Bedogni & Woodward 1990). These studies found that shocked clouds travel ∼8 cloud radii before mixing with the ambient medium as a result of hydrodynamic instabilities.…”

Section: Introductionsupporting

confidence: 69%

Hydrodynamical Coupling of Mass and Momentum in Multiphase Galactic Winds

Schneider

Robertson

2017

ApJ

150

143

View full text Add to dashboard Cite

Using a set of high-resolution hydrodynamical simulations run with the Chollacode, we investigate how mass and momentum couple to the multiphase components of galactic winds. The simulations model the interaction between a hot wind driven by supernova explosions and a cooler, denser cloud of interstellar or circumgalactic media. By resolving scales of Dx 0.1 pc over 100 pc distances, our calculations capture how the cloud disruption leads to a distribution of densities and temperatures in the resulting multiphase outflow and quantify the mass and momentum associated with each phase. We find that the multiphase wind contains comparable mass and momenta in phases over a wide range of densities and temperatures extending from the hot wind ( » -n 10 2.5 -cm 3 , » T 10 6.5 K) to the coldest components ( » n 10 2 -cm 3 , » T 10 2 K). We further find that the momentum distributes roughly in proportion to the mass in each phase, and the mass loading of the hot phase by the destruction of cold, dense material is an efficient process. These results provide new insight into the physical origin of observed multiphase galactic outflows and inform galaxy formation models that include coarser treatments of galactic winds. Our results confirm that cool gas observed in outflows at large distances from the galaxy (1 kpc) likely does not originate through the entrainment of cold material near the central starburst.

show abstract

Section: Introductionsupporting

confidence: 69%

Hydrodynamical Coupling of Mass and Momentum in Multiphase Galactic Winds

Schneider

Robertson

2017

ApJ

150

143

View full text Add to dashboard Cite

show abstract

“…In the most well known simulations ( Nittmann et al 1982;KMC;Mac Low et al 1994;Nakamura et al 2006), it is assumed that a low-density molecular cloud with no selfgravity or magnetic fields is exposed to a steady shock. The shock collides with the cloud, producing a reverse shock that develops into a bow shock; a shock propagates through the cloud, passing through it in a ''cloud crushing'' time t cc .…”

Section: This Raises the Question If Our Resolution Is Not As Good Amentioning

confidence: 99%

Interaction of Supernova Ejecta with Nearby Protoplanetary Disks

Ouellette

Desch

Hester

2007

ApJ

141

229

View full text Add to dashboard Cite

The early solar system contained short-lived radionuclides such as 60 Fe (t 1/2 = 1.5 Myr) whose most likely source was a nearby supernova. Previous models of solar system formation considered a supernova shock that triggered the collapse of the Sun's nascent molecular cloud. We advocate an alternative hypothesis, that the solar system's protoplanetary disk had already formed when a very close (<1 pc) supernova injected radioactive material directly into the disk. We conduct the first numerical simulations designed to answer two questions related to this hypothesis: Will the disk be destroyed by such a close supernova, and will any of the ejecta be mixed into the disk? Our simulations demonstrate that the disk does not absorb enough momentum from the shock to escape the protostar to which it is bound. Only low amounts (<1%) of mass loss occur, due to stripping by Kelvin-Helmholtz instabilities across the top of the disk, which also mix into the disk about 1% of the intercepted ejecta. These low efficiencies of destruction and injection are due to the fact that the high disk pressures prevent the ejecta from penetrating far into the disk before stalling. Injection of gas-phase ejecta is too inefficient to be consistent with the abundances of radionuclides inferred from meteorites. On the other hand, the radionuclides found in meteorites would have condensed into dust grains in the supernova ejecta, and we argue that such grains will be injected directly into the disk with nearly 100% efficiency. The meteoritic abundances of the short-lived radionuclides such as 60 Fe therefore are consistent with injection of grains condensed from the ejecta of a nearby (<1 pc) supernova, into an already formed protoplanetary disk.

show abstract

“…When an adiabatic cloud is impacted, it passes through four characteristic phases: compression, re-expansion, fragmentation and mixing with the ISM (see, e.g., Nittmann et al 1982;McKee 1988;Klein et al 1994). Its gas is initially compressed by an internal forward shock wave that crosses the cloud in a time t crush ∼ t SC q 0.5 , where q = ρ c /ρ sh is the ratio between the density of the cloud and the SSSF.…”

Section: Setmentioning

confidence: 99%

Multidimensional hydrodynamical simulations of radiative cooling SNRs-clouds interactions: an application to starburst environments

Melioli¹,

Pino²,

Raga³

2005

A&A

View full text Add to dashboard Cite

Most galaxies present supernova shock fronts interacting with cloudy interstellar medium. These interactions can occur either at small scales, between a single supernova remnant (SNR) and a compact cloud, or at large scales, between a giant shell of a superbubble and a molecular cloud. Here study the by-products of SNR-clouds in a starburst (SB) system. Due to the high supernova (SN) rate in this environment, a cloud may be shocked more than once by SNRs. These interactions can have an important role in the recycling of matter from the clouds to the ISM and vice-versa. Their study is also relevant to understand the evolution of the ISM density and the structure of the clouds embedded in it. In the present work, we have focused our attention on the global effects of the interactions between clouds and SN shock waves in the ISM of SB environments and performed three-dimensional radiative cooling hydrodynamical simulations which have included the continuity equations for several atomic/ionic and molecular species. We have also considered the effects of the photo-evaporation due to the presence of the UV radiation from hot stars and SNe. The results have shown that due to the presence of radiative cooling, the interactions cause the formation of elongated cold filaments, instead of favoring an efficient mixing of the cloud gas with the diffuse ISM. These filaments could be associated with the dense clumps observed inside several SBs that are blown out by the galactic wind. The results have also revealed that the SNR-cloud interactions are less efficient at producing substantial mass loss from the clouds to the diffuse ISM than mechanisms such as the photo-evaporation caused by the UV flux from the hot stars. This result has important consequences for the global evolution of the SB environment and the formation of the associated superwinds, and may also be relevant to the ISM of normal galaxies.

show abstract

The dynamical destruction of shocked gas clouds

Cited by 80 publications

References 0 publications

Hydrodynamical Coupling of Mass and Momentum in Multiphase Galactic Winds

Hydrodynamical Coupling of Mass and Momentum in Multiphase Galactic Winds

Interaction of Supernova Ejecta with Nearby Protoplanetary Disks

Multidimensional hydrodynamical simulations of radiative cooling SNRs-clouds interactions: an application to starburst environments

Contact Info

Product

Resources

About