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Prentice, A. J. R.

doi:10.1023/a:1010692812892

Cited by 14 publications

(14 citation statements)

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“…The elastic characteristics of pure water ice were studied in many works (see, e.g., [4,5]). It is known, however, that the major portion of ice in the lithospheres of the satellites of large planets and in glaciers consists of a solid solu tion of water with salts and other components at cer tain concentrations (see, e.g., [6][7][8]). In most cases, saline ice in nature exists at high pressures and low temperatures at T < 220 K. However, its elastic prop erties and stability under these conditions are poorly understood.…”

Section: Introductionmentioning

confidence: 99%

Ultralow elastic stability of salt ice at low temperatures

Fateev

2012

Tech. Phys.

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Section: Introductionmentioning

confidence: 99%

Ultralow elastic stability of salt ice at low temperatures

Fateev

2012

Tech. Phys.

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“…The present paper is concerned with the mathematical foundation of the modern Laplacian theory of Solar system origin (Prentice 1978a,b, 1996a,b, 2001a; Prentice & ter Haar 1979). This theory, dubbed the MLT, is a modern reformulation of the original nebula hypothesis of Laplace (1796) according to which the planets condensed close to their present orbital radii from a concentric system of circular gas rings.…”

Section: Introductionmentioning

confidence: 99%

A numerical simulation of supersonic turbulent convection relating to the formation of the Solar system

Prentice

Dyt

2003

Monthly Notices of the Royal Astronomical Society

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A flux-corrected transport scheme due to Zalesak is used to carry out a numerical simulation of thermal convection in a two-dimensional layer of ideal, diatomic gas, which is heated from below and stratified gravitationally across many pressure scaleheights. The purpose of this calculation is to mimic the physical conditions in the outer layers of the protosolar cloud (PSC) from which the Solar system formed. The temperature T 0 at the top boundary (z = 0) and the dimensionless temperature gradient θ = (d/T 0 )∂ T /∂z at the base of the layer of thickness d are kept fixed, with θ = 10. The initial atmosphere is uniformly superadiabatic, having polytropic index m in = 1. Because the Reynolds number of the real atmosphere is so large, a subgrid-scale (SGS) turbulence approximation due to Smagorinsky is used to model the influence of motions with length-scale less than the computational grid size.The flow soon evolves to a network of giant convective cells, which span the whole layer. At cell boundaries the downflows are spatially concentrated and rapid while the upflows are broad and sluggish. The peak downflow Mach number is M peak = 1.1 at depth z = 0.55d. The descent of the cold gas eliminates much of the initial superadiabatic structure of the atmosphere for z 0.1d, thereby reducing the long-term mean temperature gradient dT lt /dz and causing a net shift of mass towards the base.In the top 10 per cent of depth, SGS modelling causes dT lt /dz to increase sharply. A steep density inversion occurs with the long-term mean densityρ lt (0) at the top boundary rising to 3.5 times the initial density ρ 0 there. This result gives new credibility to the modern Laplacian theory (MLT) of Solar system origin. Here a postulated 35-fold density increase at the surface of the PSC causes the shedding of discrete gas rings at the observed mean orbital spacings of the planets. Even so, further numerical simulations, corresponding to higher values of θ, which may yield values M peak 3 andρ lt (0)/ρ 0 35, are required before the MLT can be considered to be valid.

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“…This value is much less than the value ~ 3.87 g/cm 3 expected at Amalthea's orbital distance, namely 2.539i?j (i?j = 71492 km), had this body formed as a native Jovian satellite. The latter density follows from a gas ring condensation model which successfully accounts both for the broad distributions of mass and orbital radius, and the bulk chemical compositions of the four large Galilean moons (Prentice & ter Haar 1979, Prentice 2001a. This model provides a condensation temperature and gas pressure at Amalthea's orbit of ~ 880 K and ~ 45 bar, respectively.…”

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confidence: 99%