Gravitational instability of a multilayered system of high viscosity by H. OdeМЃ

Cover of: Gravitational instability of a multilayered system of high viscosity | H. OdeМЃ

Published by North Holland in Amsterdam .

Written in English

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Subjects:

  • Rock deformation.,
  • Viscosity.,
  • Rock mechanics.,
  • Fluid mechanics.

Edition Notes

Book details

Statementby H. Odé.
SeriesVerhandelingen der Koninklijke Nederlandse Akademie van Wetenschappen, afd. Natuurkunde, 1. sect., deel 24, no. 1
Classifications
LC ClassificationsQ57 .A532 deel 24, no. 1, QE604 .A532 deel 24, no. 1
The Physical Object
Pagination96 p.
Number of Pages96
ID Numbers
Open LibraryOL5337488M
LC Control Number72190875

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Get this from a library. Gravitational instability of a multilayered system of high viscosity. [H Odé]. THEORY OF VISCOUS BUCKLING AND GRAVITY INSTABILITY OF MULTILAYERS WITH LARGE DEFORMATION Abstract: An exact treatment of the stability of multilayered viscous fluids in slow motion with large deformations leads to an analog model which includes the effect of gravity.

A distinction can be made between true mechanical instability and an. where C (∽ 1) is an empirical constant that depends on n, wavelength, and the nature of the density distribution (constant in the layer or linearly decreasing with depth), Δp is the density difference between the layer and the underlying half-space.B is a measure of resistance to deformation, h is the thickness of the layer, g is gravitational acceleration, t is time, and t b is the time at Cited by: Inherent gravitational instability of hot continental crust: Implications for doming and diapirism in granulite facies terrains Author(s) Taras V.

Gerya. A RT instability occurs when a dense fluid overlies a less dense fluid. Such instabilities can arise in magmatic systems when a layer of buoyant melt is trapped within a denser crystalline mush. The full dynamics of RT instability are too complex to be described by: 6.

It is argued that the lowering of the viscosity of rocks with increasing temperature after tectonic or magmatic stacking will set the stage for processes of gravitational redistribution and. Claire A. Currie, Mihai N. Ducea, Peter G. DeCelles, Christopher Beaumont, "Geodynamic models of Cordilleran orogens: Gravitational instability of magmatic arc roots", Geodynamics of a Cordilleran Gravitational instability of a multilayered system of high viscosity book System: The Central Andes of Argentina and Northern Chile, Peter G.

DeCelles, Mihai N. Ducea, Barbara Carrapa, Paul A. Kapp. Instability criterion depends on bulk properties of the flow and on wavelength of perturbation.

Instability is independent of boundary conditions. Instability is sensitive to boundary conditions. Instability is catastrophic (major overturn, mixing).

Instability is gradual (growing wave and vortex formation). Example: overturning of a top-heavy fluid. Newer three-dimensional hydrodynamic models have shown that vigorous gravitational instability can occur in a disk with a mass of solar mass or even less, in orbit around a solar-mass star (Boss, ), because of the expected low midplane temperatures (∼30 K) in the outer disk implied by cometary compositions (Kawakita et al., ) and by observations of disks (D'Alessio et al., ).

and Muchikel [13] investigated the effect of temperature-dependent viscosity on ferroconvective instability in a porous medium.

It is found that the stationary mode of instability is preferred to oscillatory mode and that the effect of temperature-dependent viscosity has a destabilizing effect on the onset of convection.

Inherent gravitational instability of hot continental crust 99 algorithm suggested by de Capitani and Brown () for complex systems containing non-ideal solid solutions.

Thermo-dynamic data for minerals and aqueous fl uid were taken from the internally consistent database of. neutrals on the gravitational instability of interstellar and interplanetary plasmas. Chonkar and Bhatia 4 have studied the combined influence of Coriolis force and viscosity on plasma stability in the absence of Hall currents and concluded that viscosity has a stabilizing influence on the system.

The suggestion that in regions of widespread crustal extension, gravitational instability of mantle lithosphere could facilitate the development of core complexes is obviously speculative.

This analysis, which exploits linear stability of a structure whose constitutive relationship is limited to Newtonian viscosity merely touches the surface of Cited by: 6. analyzed many years ago [8]. At high redshifts asso-ciated with the recombination epoch (z ’) the role played by the shear viscosity would be negligible while the bulk viscosity would be important [8].

In ad-dition, the gravitational instability for a uid which sup-ports viscoelastic stresses was addressed by. The gravitational instability of flow through porous medium for some hydrodynamical and hydromagnetical systems of astrophysical interest is investigated.

The effects of rotation, magnetic field, viscosity and finite electrical conductivity are studied for the gravitational instability through porous medium. The effect of suspended particles on the instability is also by:   A hierarchy of hydrodynamical instabilities controlling the transfer of buoyancy through the oceanic mixed layer is reviewed.

If a resting ocean of horizontally uniform stratification is subject to spatially uniform buoyancy loss at the sea surface, then gravitational instability ensues in which buoyancy is drawn from depth by upright convection.

But if spatial inhomogeneities in the ambient Cited by: The standard model of gravitational structure formation is based on the Jeans acoustic theory, neglecting nonlinear instabilities controlled by viscosity, turbulence and diffusion.

A linear insta-bility length scale equal to the sound speed times the gravitational freefall time emerges. Because the. In the present paper, we investigate the effect of rotation on the onset of gravitational collapse and the growth rate of magnetogravitational instability of a finitely electrically conducting viscoelastic medium under both strongly and weakly coupled plasma limits for transverse and longitudinal modes of wave by: 3.

Figure 5 has been plotted between the normalized growth rate and the normalized wave number to examine the effect of shear viscosity on the Jeans instability of a viscoelastic fluid taking, and we found that the growth rate is decreasing on increasing the value of which indicates the stabilizing effect of shear by: 3.

The viscosity and specific gravity of the liquids have been measured as follows: Viscosity of glucose syrup = Pa-S, Viscosity of oil = Pa-S, Specific Gravity of Glucose syrup =Specific Gravity of oil = 4.

Experimental Technique. In the experiment, first the setup rests at position 3 where the light fluid lies over the heavy : Snehamoy Majumder, Debajit Saha, Partha Mishra. Simple 2-D, two-layer gravity instability modelling of diapir wavelengths and growth rates has determined values of approximately to for the ratio of equivalent viscosity of the overburden.

Books. Gerya, T.V., Dacenko, V.M., Zablotsky, K.A., Kornev,Lepezin, G.G., Nozhkin, A.D., Popov, N.V., Reverdatto, V.V., Shvedenkov, () Precambrian. The gravitational instability problem is of central importance in understanding the process of forma-tion of stars, planets, comets, asteroids and other astrophysical objects.

Initially Jeans[13] considered the gravitational instability of non-viscous ideal fluid and showed that the system. This book has been cited by the following publications. Gerya, T. V., Perchuk, L. L., Maresch, W. and Willner, A.

( c) Inherent gravitational instability of hot continental crust: implication for doming and diapirism Melnik, O. () Dynamics of two-phase conduit flow of high viscosity gas-saturated magma: large variations of Cited by:   Stress reaches a maximum at ∼4 Myr for a high-viscosity crust and at ∼ Myr for a low-viscosity crust and drop afterwards.

Differences in timing stem from the fact that a weak crust results in a more deformable upper boundary, enhancing growth of the RT by: A. Gravitational instability in layered systems 2) Parker and McDonell have shown experimentally that, for two materials of different densities with common interface, a gravitational instability will result whenever the more dense material is placed on top of a less dense one and that it is not necessary for the viscosity.

The linear self-gravitational instability of finitely conducting, magnetized viscoelastic fluid is investigated using the modified generalized hydrodynamic (GH) model. A general dispersion relation is obtained with the help of linearized perturbation equations using the normal mode analysis and it is discussed for longitudinal and transverse Cited by:   However, similar material viscosity at different altitudes will produce different effects on a body moving through the fluid field, due to a difference in air pressure.

Less viscosity effects will be present with less air pressure. On different planets (different gravity), the differences in effect. Viscous fingering is a flow instability induced by the displacement of a more viscous fluid (MVF) by a less viscous fluid (LVF) in a porous medium [1,2,3,4,5,6,7,8].The front of the miscible fluids or the interface between the immiscible fluids becomes unstable, and several fingers appear, modifying the regular pattern of the interface and thus decreasing the displacement : Tetsuya Suekane, Tomotaka Koe, Pablo Marin Barbancho.

Specific gravity is the heaviness of a substance compared to that of water, and it is expressed without units. In the metric system specific gravity is the same as in the English system.

If something is times as heavy as an equal volume of water (such as iron is) its specific gravity is @article{osti_, title = {Gravitational instabilities of superspinars}, author = {Pani, Paolo and Barausse, Enrico and Berti, Emanuele and Cardoso, Vitor and Maryland Center for Fundamental Physics, Department of Physics, University of Maryland, College Park, Maryland and Department of Physics and Astronomy, University of Mississippi, University, Mississippi and Centro.

Gravitational Instability in a Ferromagnetic Fluid Saturated Porous Medium with Non-Classical 12 | Page where o f Pr is the Prandtl number, 2 1 d Da k is the inverse Darcy number, f f is the Brinkman number, 4 o f g d R is the thermal Rayleigh number, o= 1 2 2 4K d N f is the magnetic Rayleigh number, = 22 C d is the.

The initial linear phase of a streaming instability, begins with a transient region of high pressure within the protoplanetary disk. The elevated pressure alters the local pressure gradient supporting the gas, reducing the gradient on the region's inner edge and increasing the gradient on the region's outer edge.

Explanation. We are given the mass of the baseball outside of the water. Using the weight equation with the gravitational constant being and the mass being, the weight of the baseball outside of the water is N. (Be careful and convert the mass of the baseball from grams to kilograms since we are using SI units).

The buoyancy force is the difference of the weight of the baseball when. The stability of an n‐layered liquid film flowing steadily down an inclined plane is investigated using linear theory.

Neutral curves of all competing modes of instability have been obtained for various ratios of viscosity, density, and thickness. The interfacial mode instability due to the local downward step increase in density is found to occur only when such a density increase is large Cited by: 1 Introduction.

Venus provides an interesting conundrum for planetary science. Venus is only slightly smaller than Earth; they have similar mean densities and moments of inertia, indicating that the two have similar internal structures and internal compositions [Solomon and Head, ].It would follow that Venus has a mantle density and viscosity structure similar to Earth's as well.

The Origin of the Earth and by gravitational instability. It also provides an explanation of the differences between planetary bodies in the solar system and explains the differences between the heavier terrestrial planets close to the sun, and the lighter, more gaseous planets situated at a.

The main focus of this video is the role of viscosity in stabilizing such a system and dampen out relative velocity. This, in the end, leads to rigid body rotation, even though the early system. Experiments and Simulations of a Gravitational Granular Flow Instability Jan Ludvig Vinningland,1, ∗ Øistein Johnsen,1 Eirik G.

Flekkøy,1 Renaud Toussaint,2 and Knut Jørgen Måløy1 1Department of Physics, University of Oslo, P. Oslo, Norway 2Institut de Physique du Globe de Strasbourg, CNRS, Université Louis Pasteur, 5 rue Descartes, Strasbourg Cedex, France.

The selection of legs as “master” and “slave” influences the system’s stability (see section Gravitational Instability) and impacts a system’s dynamic behavior. Dynamic performance is very important in semiconductor inspection machines which have fast moving : TMC Vibration Control.

The scaled gravitational constant, or Einstein's constant, is: κ = 8π / c 4 G ≈ × 10 −43 s 2 ⋅m −1 ⋅kg −1.

Value and dimensions. The gravitational constant is a physical constant that is difficult to measure with high accuracy. This is because the gravitational force is extremely weak as compared to other fundamental forces.Dear Colleagues, Many practical problems involving porous media in engineering, geophysics and CO 2 sequestration involve the simulation of what might be termed convection in a very wide sense.

Such instabilities are always brought about by nonuniform buoyancy forces due to density changes which, in turn, have arisen because of variations in the temperature and/or chemical composition of the.The importance of gravitational instability in determining the emulsification of vitreal tamponades is discussed.

Theoretical results and numerical simulations indicate that the spontaneous formation of water-silicon oil is a rare event and that the very low concentration of surface active agents cannot justify the systematic formation of by: 2.

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