A possible solution to the problem of the Galactic evolution of D and He-3

Details A possible solution to the problem of the Galactic evolution of D and He-3 A possible solution to the problem of the Galactic evolution of D and He-3

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...432l.101g&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 432, no. 2, p. L101-L104

Computer Science

Numerical Analysis

18

Abundance, Big Bang Cosmology, Deuterium, Galactic Evolution, Helium Isotopes, Nuclear Fusion, Nuclear Reactions, Stellar Evolution, Stellar Models, Baryons, Chemical Evolution, Numerical Analysis, Photons, Ratios, Stellar Mass

Scientific paper

Light elements, and in particular D and He-3, are commonly used as cosmological probes to obtain bounds on the baryon-to-photon ratio, eta, and to test the predictions of big bang nucleosynthesis. Current models of stellar evolution predict a production of He-3 in stars of low and intermediate mass that, when averaged over the Galactic lifetime, leads to a strong inconsistency between observed and model abundances. In this Letter, we suggest a solution to the problem of the overproduction of He-3 based on nuclear physics. In particular, we consider the effects that a low-energy resonance in the cross section of the He-3 + He-3 reaction has on the stellar yields of stars of different masses. We then follow the evolution of D and He-3 using a model for the chemical evolution of the Galactic disk. We show that, if the energy of the resonance is below Er approximately equal to 10 keV, an excellent agreement between the solar system data and the model predictions is found. We also derive stringent bounds on eta: 3.5 less than or = eta10 less than or = 4.5. Conversely, one can use the observed solar abundances to constrain the resonance properties.

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