Cosmological helium production simplified

Jeremy Bernstein, Lowell S. Brown, and Gerald Feinberg
Rev. Mod. Phys. 61, 25 – Published 1 January 1989
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Abstract

The authors present a simplified model of helium synthesis in the early universe. The purpose of the model is to explain clearly the physical ideas relevant to the cosmological helium synthesis in a manner that does not overlay these ideas with complex computer calculations. The model closely follows the standard calculation, except that it neglects the small effect of Fermi-Dirac statistics for the leptons. The temperature difference between photons and neutrinos during the period in which neutrons and protons interconvert is also neglected. These approximations permit the expression of neutron-proton conversion rates in a closed form, which agrees to 10% accuracy or better with the exact rates. Using these analytic expressions for the rates, the authors reduce the calculation of the neutron-proton ratio as a function of temperature to a simple numerical integral. They also estimate the effect of neutron decay on the helium abundance. Their result for this quantity agrees well with precise computer calculations. Their semianalytic formulas are used to determine how the predicted helium abundance varies with such parameters as the neutron lifetime, the baryon-to-photon ratio, the number of neutrino species, and a possible electron-neutrino chemical potential.

    DOI:https://doi.org/10.1103/RevModPhys.61.25

    ©1989 American Physical Society

    Authors & Affiliations

    Jeremy Bernstein*

    • Department of Physics, Stevens Institute of Technology, Hoboken, New Jersey 07030 and The Rockefeller University, Department of Physics, New York, New York 10021-5399

    Lowell S. Brown

    • Department of Physics, University of Washington, Seattle, Washington 98195

    Gerald Feinberg

    • Department of Physics, Columbia University, New York, New York 10027

    • *Permanent address.

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    Issue

    Vol. 61, Iss. 1 — January - March 1989

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