Titlebook: Stellar Rotation; Proceedings of the I Arne Slettebak Conference proceedings 1970 D. Reidel Publishing Company, Dordrecht, Holland 1970 sta

CRUMB

The Effects of Rotation on the Atmospheres of Early-Type Main-Sequence Stars (Review Paper)s of astrophysics and to interconnect them in a cohesive pattern structured so as to provide insight into a rather specific problem — namely, the structure and characteristics of a surface of the star undergoing axial rotation. Many different connections are possible having varying degrees of emphas

minimal

On the Effect of Rotation on Stellar Absorption Linesor the strong lines Mg. 4481 and Si. 4128, the effect may be significant for the weak ones, especially those of the Eu.-type. Because the mean atmospheric parameters of a rapidly rotating star seen pole-on are very similar to those of a non-rotating star of the same mass, this may cause significant

联邦

obeisance

Rotating Stellar Atmospheres and the Energy Distribution of Altair of these models are discussed. A specific model for the rapidly rotating star Altair has been constructed matching the observed radius, luminosity, and projected rotational velocity. It is found that the energy distribution predicted for the model agrees well with that observed for Altair, after th

Apoptosis

LAVE

Evolution of Rapidly Rotating B-Type Starse stars for which the most rapid rotation along the main sequence is observed, not a single interior model has yet been computed except in this conference reported by Kippenhahn and Thomas (1970). It is this gap that the present paper attempts to close.

headlong

tember 8th through 11 th, 1969. Forty-four scientists from Argentina, Belgium, Canada, England, Finland, East and West Germany, Italy, Israel, Japan, The Netherlands, and the United States attended and participated in the Colloquium. The present volume, which parallels the actual program closely, co

sacrum

A Simple Method for the Solution of the Stellar Structure Equations Including Rotation and Tidal For Although it is similar to that of Faulkner .. (1968) in the case of purely rotating stars, it is not necessary to use the division into two zones, where either slow rotation or negligible contribution to the gravitional potential is assumed.

Diskectomy

Rotational Perturbation of a Radial Oscillation in a Gaseous Starighboring nonrotating configuration. Care has also been taken, in the perturbation method, to account for the existence of the so-called ‘trivial modes’ of the sphere, i.e. those oscillations of vanishing frequencies in which the displacement is transversal and divergence-free.

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