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

FRONT

Accuracy tests for the computation of solar models,We discuss the choice of the difference scheme and of the variables. We also show that a slight modification to the usual difference method allows a significant increase of the accuracy and the computation of, a solar model with a reasonable number of meshpoints.

大溝

Comparison of solar models with Los Alamos and Livermore opacities,Models of the present sun were computed using the Los Alamos and the new Livermore opacities. The relative abundance abundance of heavy elements was the Grevesse mixture and the ratio Z/X was taken as 0.02765. The models were iterated to have R = R. and L = L. at an age of t. = 4.6 10. years. The differences between the two models are presented.

EWE

Interlocking

Conference proceedings 1991nsitivity of oscillationsto uncertainties in fundamental physics, and thestudy ofthe angular velocity and the dynamics of the convectionzone.Of particular interest is the structure of the solarcore and its relevance to the neutrino problem. Theunderstanding so gained permits one to lookaheadconfiden

Organonitrile

0075-8450 t of thesensitivity of oscillationsto uncertainties in fundamental physics, and thestudy ofthe angular velocity and the dynamics of the convectionzone.Of particular interest is the structure of the solarcore and its relevance to the neutrino problem. Theunderstanding so gained permits one to lookahe

削減

谷物

https://doi.org/10.1007/978-3-642-30001-1ity for separating different contributions to the difference between the models, on the basis of the frequencies of the modes. Analysis of observed frequencies suggests that the solar envelope helium abundance .. is close to 0.25; however, this result may be sensitive to other uncertainties in the solar models.

ARIA

Frisky

Influence of the upper layers of the sun on the p-mode frequencies,ity for separating different contributions to the difference between the models, on the basis of the frequencies of the modes. Analysis of observed frequencies suggests that the solar envelope helium abundance .. is close to 0.25; however, this result may be sensitive to other uncertainties in the solar models.

Exposition