Diffusion in the Sun.

Aller, L. H.; Chapman, S.

doi:10.1086/146943

Cited by 105 publications

(56 citation statements)

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“…Di †erent authors employ di †erent notations, e.g., equation (2.1) of Aller & Chapman (1960), equation (3) of Schatzman (1969), equation (1) of Michaud (1970), and equation (1) of Vauclair & Vauclair (1982). As one can see from equation (45), is J i contributed not only by the gradient of the concentration, a reasonable approximation under laboratory situations, but also by temperature and pressure gradients, Ðrst introduced by Chapman (1917), which may be important in stellar interiors.…”

Section: Concentration Equationsmentioning

confidence: 99%

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Turbulence in Stars. III. Unified Treatment of Diffusion, Convection, Semiconvection, Salt Fingers, and Differential Rotation

Canuto

1999

ApJ

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Section: Concentration Equationsmentioning

confidence: 99%

“…In the absence of turbulence, di †usion was studied by Aller & Chapman (1960), Michaud (1970), Vauclair & Vauclair (1982), and Bahcall & Pinsonneault (1992). Schatzman (1969Schatzman ( ), (1996 and Schatzman & Baglin (1991) attempted to include turbulence via an enhanced di †usion coefficient.…”

Section: The Case Of a Passive Scalarmentioning

confidence: 99%

Turbulence in Stars. III. Unified Treatment of Diffusion, Convection, Semiconvection, Salt Fingers, and Differential Rotation

Canuto

1999

ApJ

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“…Often, in the literature, J i includes the density and has the opposite sign and χ c is called D. We also note that different authors have used different notations, e.g., Eq. (2.1) of Aller & Chapman (1960), Eq. (3) of Schatzman (1969), Eq.…”

Section: Passive Tracer Fluxmentioning

confidence: 99%

Stellar mixing

Canuto

2011

A&A

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In Papers I-II, we derived the expressions for the turbulent diffusivities of momentum, temperature T , and mean molecular weight μ. Since the scalar T -μ fields are active tracers (by influencing the density and thus the velocity field), whereas passive tracers such as 7 Li are carried along by the flow without influencing it, it would be unjustified to use the diffusivities of the T -μ fields to represent the diffusivity of passive tracers. In this paper, we present the first derivation of a passive tracer diffusivity. Some key results are: a) In the general 3D case, the passive tracer diffusivity is a tensor given in algebraic form; b) the diffusivity tensor depends on shear, vorticity, T , and μ-gradients, thus including double diffusion and differential rotation; c) in the 1D version of the model, the passive tracer diffusivity is a scalar denoted by K c ; d) in doubly stable regimes, ∇ μ > 0, ∇ − ∇ ad < 0, K c is nearly the same as those of the T -μ fields; e) in semi-convection regimes, ∇ μ > 0, ∇ − ∇ ad > 0, K c is larger than that of the μ-field; f) in salt fingers regimes ∇ μ < 0, ∇ − ∇ ad < 0, K c is smaller than that of the μ-field; and finally, g) in the only case we know of a direct measurement of a passive tracer diffusivity, the oceanographic North Atlantic Tracer Release Experiment (NATRE), the model reproduces the data quite closely.

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“…In the case of a test particle (of very small abundance) in completely ionized hydrogen Aller and Chapman (1960) computed the electric field and obtained the velocity of diffusion of an ionized test-particle assuming that the only forces acting are the electric and gravitational forces. This treatment is justified for A stars as the outerlayers are almost completely devoid of.…”

Section: Dramentioning

confidence: 99%

Rotation Mixing and Variability in a Stars

Baglin

1976

International Astronomical Union Colloquium

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A. B a g l i n O b s e r v a t o i r e de N i c e , Le Mont-Gros, 06 300 NiceThe purpose of this paper is to contribute to answer the question : why among A stars are there variable and "constant" stars ? To do this we will f i r s t review the observational properties of these s t a r s , then discuss the theoretical models based on the interplay between microscopic diffusion and rotation, and finally discuss the "unsolved" questions ! AReview of the properties of the A stars in the instability strip Ci.e. on the main sequence from A2 to FO, and somewhat l a t e r types in giants] .

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Diffusion in the Sun.

Cited by 105 publications

References 0 publications

Turbulence in Stars. III. Unified Treatment of Diffusion, Convection, Semiconvection, Salt Fingers, and Differential Rotation

Turbulence in Stars. III. Unified Treatment of Diffusion, Convection, Semiconvection, Salt Fingers, and Differential Rotation

Stellar mixing

Rotation Mixing and Variability in a Stars

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