Hostname: page-component-f7d5f74f5-dcd55 Total loading time: 0 Render date: 2023-10-04T11:28:59.378Z Has data issue: false Feature Flags: { "corePageComponentGetUserInfoFromSharedSession": true, "coreDisableEcommerce": false, "coreDisableSocialShare": false, "coreDisableEcommerceForArticlePurchase": false, "coreDisableEcommerceForBookPurchase": false, "coreDisableEcommerceForElementPurchase": false, "coreUseNewShare": true, "useRatesEcommerce": true } hasContentIssue false

On the possible directions of evolutionary trends of stars in the Hertzsprung-Russel diagram

Published online by Cambridge University Press:  14 August 2015

V. Krat*
Pulkovo Observatory, Leningrad, URSS.


Core share and HTML view are not possible as this article does not have html content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The evolution of a star depends on the initial conditions existing during its formation and on the course of the main processes changing its chemical composition and mass. If it is assumed that stars are formed from diffuse matter, the initial conditions are restricted to three factors: 1) mass, 2) chemical composition, 3) angular momentum. The mass of the star can be determined by the conditions of gravitational instability of diffuse matter, which, according to our hypothesis, consisted of solid primary bodies, similar to cometary nuclei, and a gas and dust nebula formed by them. The upper limit for the possible mass of a star is evidently determined by its angular momentum, which cannot exceed a certain critical value.

II. Theoretical Interpretations of the Hertzsprung-Russell Diagram
Copyright © CNRS 1959 


[1] Krat, V. A., Poulk. Obs. Bull. No. 145, 1950.Google Scholar
[2] Krat, V. A., Poulk. Obs. Bull. No. 149, 1952.Google Scholar
[3] Ruskol, E. L., A. J. USSR 32, 3, 1955.Google Scholar
[4] van d. Hulst, H. C., Utrecht Rech. 11, 11, 1949.Google Scholar
[5] Kosyrev, N. A., Publ. Krim. Astroph. Obs. 6, 54, 1951.Google Scholar
[6] Krat, V. A., C R de l'Ac. Sc. de l'URSS, 86, 1081, 1952.Google Scholar
[7] Krat, V. A., Poulk. Obs. Bull. No. 156, 1956; Problems of Cosmogony, 5, 47, 1957.Google Scholar
[8] Krat, V. A., Comm. Symp. Non-Stable Stars, Ac. Sc. USSR, 1955.Google Scholar
[9] Kuiper, G. P., Ap. J. 93, 133, 1940.CrossRefGoogle Scholar
[10] Jeans, J., Astronomy and Cosmogony, Cambridge, 1928.Google Scholar
[11] Krat, V. A., Figures of Equilibrium of Celestial Bodies, Moscow - Leningrad, 1950.Google Scholar
[12] Opik, E., Les processus nucléaires dans les astres, Comm. au cinquième Coll. Int. Liège, p. 11, 1954.Google Scholar