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The Formation of Li, Be, B Isotopes by the Spallation of CNO

Published online by Cambridge University Press:  30 March 2016

E. Gradsztajn
E. Gradsztajn*
Affiliation:
Institut de Physique Nucléaire, Orsay, France

Extract

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In 1955 Fowler et al. (1955) suggested that the elements Li, Be and B could be produced at the surface of some stars by the spallation of CNO induced by electromagnetically accelerated particles.

Since that time many observational data were gathered, not only on the lithium elemental abundance (Hunger, 1957; Bonsack and Greenstein, 1960), but also concerning the isotopic ratio 7Li/6Li (Herbig, 1964; Wallerstein, 1965). Then, the abundance of beryllium in many stars was measured (Bonsack, 1960; Conti and Danziger, 1966; Merchant, 1966) and the problem was, and still is to explain both 7Li/6Li and Li/Be ratios. In addition to spallation, different possibilities may be invoked, such as the inheritance from galactic gas enriched with matter remaining from a previous generation of stars, or from the big bang; but which can be checked most easily at the present time is the spallation assumption. Indeed, simultaneously with the development of the observations on stars, a program for measuring and calculating the production rates of the light elements has been in progress at Orsay. In 1960 the first experimental result concerning the production of 6Li in 16O by 156 MeV protons was obtained. But it was only in 1965 that the number of experimental and theoretical data on spallation was sufficient to make a valid comparison with abundances observed on the stars as well as in the solar system or in cosmic rays.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 1: Highlights of Astronomy. As presented at the XIIIth General Assembly of the IAU, 1967 , 1968 , pp. 251 - 254
Copyright
Copyright © Reidel 1968

References

Bernas, R., Epherre, M., Gradsztajn, E., Klapisch, R., Yiou, F. (1965) Phys. Rev. Letters, 15, 147.Google Scholar
Bonsack, W.K.,Greenstein, J.L. (1960) Astrophys. J., 131, 83.CrossRefGoogle Scholar
Bonsack, W.K. (1960) Astrophys. J., 133, 551.Google Scholar
Conti, P.S., Danziger, I.I. (1966) Astrophys. J., 146, 383.CrossRefGoogle Scholar
Cumming, J.B. (1963) Am. Rev. Nucl. Sci., 13, 261.Google Scholar
Dostrovsky, I., Fraenkel, Z., Rabinowitz, P. (1958) Phys. Rev., 118, 791.Google Scholar
Epherre, M., Gradsztajn, E. (1967) J. Phys., 28, 745.Google Scholar
Fowler, W.A., Burbidge, G.R., Burbidge, E.M. (1955) Astrophys. J., Suppl., 2, 167.Google Scholar
Herbig, G. (1964) Astrophys. J., 140, 702.Google Scholar
Hunger, K. (1957) Astron. J., 62, 294.Google Scholar
Merchant, A. (1966) Astrophys. J., 143, 336.Google Scholar
Metropolis, N., Bivins, R., Storm, M., Miller, J.M., Friedlander, G.,Turkevitch, A. (1958) Phys. Rev., 110, 185.Google Scholar
Reeves, H. (1967) Unesco Conf. on the Origin and Abundance of the Elements, Paris, May 1967.Google Scholar
Rudstam, G. (1956) Thesis, Uppsala.Google Scholar
Serber, R. (1947) Phys. Rev., 72, 1114.Google Scholar
Wallerstein, G. (1965) Astrophys. J., 141, 311.CrossRefGoogle Scholar
Yiou, F., Baril, M., Dufaure de Citres, J., Fontes, P., Gradsztajn, E., Bernas, R. (1968) Phys. Rev., 166, 968.CrossRefGoogle Scholar