Numerical Simulations of Deep Nonlinear Richtymer‐Meshkov Instability

Graham, Mary Jane; Zhang, Qiang

doi:10.1086/313346

Cited by 12 publications

(10 citation statements)

References 5 publications

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“…The clumped and fragmented morphology of the GC region strongly suggests that it has been shaped by a supersonic turbulence generated by the shocks implied in the modelling (Paper I). Shocks are known to produce turbulence, notably via the Richtmyer–Meshkov instability which is due to the shock acceleration, and is similar to the familiar Raleigh–Taylor instability (see e. g. Mikaelian 1990; Graham & Zhang 2000). Shocks can also lead to other instabilities, e.g.…”

Section: Discussionmentioning

confidence: 99%

“…Shocks are known to produce turbulence, notably via the Richtmyer–Meshkov instability which is due to the shock acceleration, and is similar to the familiar Raleigh–Taylor instability (see e.g. Mikaelian 1990; Graham & Zhang 2000). Shocks can also lead to other instabilities e.g.…”

Section: Turbulence Abundance Fluctuations and Magnetic Fieldmentioning

confidence: 99%

“…7 This is an important issue revealing that matter is highly fragmented. It could be a result of Richtmyer-Meshkov (RM) ( Mikaelian 1990;Graham & Zhang 2000) instability which is an interfacial instability between two fluids of different densities driven by weak and intermediate shock waves characteristically leading to photoionized "fingers". (For a discussion of the fragmentation generated by Kelvin-Helmholtz instablities, see Sect.…”

Section: Optical Linesmentioning

confidence: 99%

“…The analysis presented in Paper I invoked the existence of shocks as a necessary ingredient for a consistent derivation of the spectra observed by Simpson et al (2007). Shocks are known to produce turbulence, notably via the Richtmyer-Meshkov instability which is due to the shock acceleration, and is similar to the familiar Raleigh-Taylor instability (see e. g. Mikaelian 1990;Graham & Zhang 2000 ). Shocks can also lead to other instabilities e.g.…”

Section: Turbulence Abundance Fluctuations and Magnetic Fieldmentioning

confidence: 99%

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Spectra from the shocked nebulae revealing turbulence near the Galactic Centre

Contini¹,

Goldman²

2010

Monthly Notices of the Royal Astronomical Society

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The spectra emitted from clouds near the Galactic Centre (GC) are investigated calculating the UV–optical–IR lines using the physical parameters and the element abundances obtained by the detailed modelling of mid‐IR observations. Graphical representation of the spectra reveals strong lines. Characteristic line ratios calculated at the nebula provide information about the dereddened spectra emitted from regions near the GC. These line ratios are compared with those observed in active galaxies. We have found that the physical conditions in the nebulae near the GC are different from those of starburst galaxies and active galactic nuclei, namely, gas velocities and densities as well as the photoionization fluxes are relatively low. The geometrical thickness of the emitting filaments is particularly small suggesting that matter is strongly fragmented by instabilities leading to an underlying shock‐generated turbulence. This is revealed by the power spectra of the radial velocities, of the mid‐IR continuum flux and of the computed Si/H relative abundances. Moreover, turbulence could amplify the initial magnetic fields.

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Section: Discussionmentioning

confidence: 99%

Section: Turbulence Abundance Fluctuations and Magnetic Fieldmentioning

confidence: 99%

Section: Optical Linesmentioning

confidence: 99%

Section: Turbulence Abundance Fluctuations and Magnetic Fieldmentioning

confidence: 99%

See 2 more Smart Citations

Spectra from the shocked nebulae revealing turbulence near the Galactic Centre

Contini¹,

Goldman²

2010

Monthly Notices of the Royal Astronomical Society

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“…The strong resemblence between the "crab legs" which appear in the He2-104 image (Fig. 1) and the boundary of the shock front presented by Graham & Zhang (2000) and, particularly, by Gull (1975, Fig. 3 ii) suggests that the "legs" are actually formed by R-T instability.…”

Section: The "Crab Legs"mentioning

confidence: 91%

Internal and external shock fronts in He2-104

Contini

Formiggini

2001

A&A

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Comparison of dust‐to‐gas ratios in luminous, ultraluminous, and hyperluminous infrared galaxies

Contini

2007

Astron Nachr

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19 pages+ 7 figures. in press in ANInternational audienceThe dust-to-gas ratios in three different samples of luminous, ultraluminous, and hyperluminous infrared galaxies are calculated by modelling their radio to soft X-ray spectral energy distributions (SED) using composite models which account for the photoionizing radiation from H II regions, starbursts, or AGNs, and for shocks. The models are limited to a set which broadly reproduces the mid-IR fine structure line ratios of local, IR bright, starburst galaxies. The results show that two types of clouds contribute to the IR emission. Those characterized by low shock velocities and low preshock densities explain the far-IR dust emission, while those with higher velocities and densities contribute to the mid-IR dust emission. Clouds with shock velocities of 500 km s-1 prevail in hyperluminous infrared galaxies. An AGN is found in nearly all of the ultraluminous infrared galaxies and in half of the luminous infrared galaxies of the sample. High IR luminosities depend on dust-to-gas ratios as high as ?0.1 by mass, however most hyperluminous IR galaxies show dust-to-gas ratios much lower than those calculated for the luminous and ultraluminous IR galaxies

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Numerical Simulations of Deep Nonlinear Richtymer‐Meshkov Instability

Cited by 12 publications

References 5 publications

Spectra from the shocked nebulae revealing turbulence near the Galactic Centre

Spectra from the shocked nebulae revealing turbulence near the Galactic Centre

Internal and external shock fronts in He2-104

Comparison of dust‐to‐gas ratios in luminous, ultraluminous, and hyperluminous infrared galaxies

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