Titlebook: Challenges to Theories of the Structure of Moderate-Mass Stars; Proceedings of a Con Douglas Gough,Juri Toomre Conference proceedings 1991

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他很靈活

Phanerozoic Phosphorite Depositional Systemsrequired to reproduce the results. A good fit was obtained with a kinetic energy spectrum which peaks at ? } 100 and decreases exponentially out to ? } 500 with an e-folding range of Δ? } 90. A power law fit to the spectrum over this range in ? yields an exponent of about ?2.75. No corrections for s

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Challenges to Theories of the Structure of Moderate-Mass StarsProceedings of a Con

Cpap155

Helium gravitational settling below the solar convection zone,olar outer layers by as much as 20% in the standard models. However the necessity of explaining also the lithium destruction in the sun and solar type stars reduces the expected helium depletion to a few percent.

儲備

Helioseismic inversion,ructure and dynamics of the solar interior. Some basic concepts and a few inversion techniques are discussed. Results on solar rotation and radial stratification are reviewed, and finally the potential for investigating other moderate-mass stars seismologically is considered.

清澈

On the 2-dimensional rotational inversion problem,the forward and inverse problem, in both the 1-dimensional case (with possible expansion in latitude and the full 2-dimensional case. Some preliminary results of running these programs are presented here, together with an outline of the whole package.

清澈

Clumsy

Prospects of solar Quantum Chaos,distribution of the spacings violates the Poisson distribution, which should hold under conditions of spherical symmetry of the equilibrium state of the sun. The relevance of this result in connection with inversion problems is briefly emphasised.

吵鬧

Granulation: Non-adiabatic patterns and shocks,ions of the solar granulation, and illustrate the corresponding pressure and velocity fields. In particular, the non-adiabatic part of the pressure fluctuation, which is a major source of stochastic excitation of P-modes, is shown.

quiet-sleep

Theoretical spectrum of solar convection, by linearly superposing these modes to yield the model convective flux profile. The numerical results are compared with the observed spectrum of solar convection and the technique is applied to other stars.