By Hubert Reeves (auth.), Jean Audouze, Nicole Mathieu (eds.)
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1. INTRODUCTION If the production and destruction of 3He in the course of galactic evolution were known, the presently observed interstellar and/or solar system abundances could be extrapolated back to prega1actic epochs. Since any deuterium processed through stars is converted to 3He via radiative proton capture, the evolution of 3He may permit bounds to be set on the primordial abundance of D ~ 3He (Yang et a1. 1984). If the destruction of 3He can be constrained, significant lower limits to the nucleon density - critical to questions of dark matter and the number of light neutrinos (or, other lIinosll) - may be 37 1.
Blake, J. B•• , Hainebach, K. C. and Schramm, D. N. 1978, Ap. J. 223, 552. Dearborn, D. S. , Schramm, D. N. and Steigman, G. 1985, Ap. J. (Submitted, May 1985). Iben, I. 1967, Ap. J. 147, 624. Iben, I. and Truran, J:'W. 1972, Ap. J. 220, 980. Rood, R. T. 1972, Ap. J. 177, 681. ---Rood, R. , Steigman, G. and Tinsley, B. M. 1976, Ap. J. ) 207, L57. Rood, R. , Bania, T. M. and Wilson, T. L. 1984, Ap. J. 280, 629. Sal peter, Eo E. 1955, Ap. J. 121, 161. , Turner, M. , Schramm, D. N. and Olive, K.
DELBOURGO-SALVADOR ET AL. 20 Fig. VI Canparison bet\oJeen the liqht elanents abundances canputed and the observed abundances (boxes) taking into account chemical evolution models with 10. 3 10- 4 • The effect of the production factor K is the same as in the case (1). But one could explain the dispersion of 3 He ~easurement by the presence of young stars ejecting 0 free and He rich and then avoid the difficulties outlined in case (i). ) models of galactic evolution implying elther the lnfall (or inflow) of processed interstellar material or preferably significant stellar mass losses occuring during the pre main sequence phase lead to Dp/Dn ratios consistent both with the 3 He and 4He abundances in the frame of the classical Big Bang nucleosynthesis (figure VI).