Abstract
It seems obvious that the sun was much more active in its early days - the T-Tauri phase, than today - the Main-sequence phase. This period of activity would have taken place before solidification in the solar system. The high degree of homogeneity of the 7Li/6Li ratio in the earth and in meteorites proves this.
Various radioactive isotopes could have been generated by the early solar proton irradiation induced by this activity. Among these isotopes, some have a half-life long enough to have been trapped eventually in the solidification of various bodies in the solar system, and may have been responsible for the early heating of the meteorites.
The most efficient radioactive heaters would be those with a half-life comparable to the period from the end of the irradiation until the beginning of solidification in the solar system. It is of course very difficult to specify this period, but it can reasonably be given limits of 105-107 years. In this respect two important isotopes are 10Be and 26A1. We use information on this early irradiation to study the importance of these heaters as compared with others such as 40K, 129I, 235U, 238U, and 244Pu.
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© 1969 D. Reidel Publishing Company, Dordrecht, Holland
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Reeves, H., Audouze, J. (1969). Heat Generation in Meteorites During the Early Stage of the Solar System. In: Millman, P.M. (eds) Meteorite Research. Astrophysics and Space Science Library, vol 12. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-3411-1_27
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DOI: https://doi.org/10.1007/978-94-010-3411-1_27
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