Galactic Evolution Of D And 3He Including Stellar Production Of 3He

Abstract

New stellar models which track the production and destruction of ${}^3$He (and D) have been evolved for a range of stellar masses $(0.65\le M/M_{\odot }\le 100)$, metallicities $(0.01\le Z/Z_{\odot }\le 1)$ and initial (main sequence) ${}^3$He mass fractions $(10^{-5}\le X_{3,MS}\le 10^{-3})$. Armed with the ${}^3$He yields from these stellar models we have followed the evolution of D and ${}^3$He using a variety of chemical evolution models with and without infall of primordial or processed material. Production of new ${}^3$He by the lower mass stars overwhelms any reasonable primordial contributions and leads to predicted abundances in the presolar nebula and/or the present interstellar medium in excess of the observationally inferred values. This result, which obtains even for zero primordial D and ${}^3$He, and was anticipated by Rood, Steigman \& Tinsley (1976), is insensitive to the choice of chemical evolution model; it is driven by the large ${}^3$He yields from low mass stars. In an attempt to ameliorate this problem we have considered a number of non-standard models in which the yields from low mass stars have been modified. Although several of these non-standard models may be consistent with the ${}^3$He data, they may be inconsistent with observations of ${}^{12}$C/${}^{13}$C, ${}^{18}$O and, most seriously, the super-${}^3$He rich planetary nebulae (Rood, Bania \& Wilson 1992). Even using the most extreme of these non-standard models (Hogan 1995), we obtain a generous upper bound to pre-galactic ${}^3$He: X${}_{3P}\le 3.2\times 10^{-5}$ which, nonetheless, leads to a stringent lower bound to the universal density of nucleons.

21 pages, plus 10 figures, accepted by ApJ

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