Three-body Effects for the p(pe^-, ν_e)d Reaction in Nuclear Astrophysics.

Details Three-body Effects for the p(pe^-, ν_e)d Reaction in Nuclear Astrophysics. Three-body Effects for the p(pe^-, ν_e)d Reaction in Nuclear Astrophysics.

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..may.c1003k&link_type=abstract

American Physical Society, APS/AAPT Joint Meeting, May 2-5, 1996, abstract #C10.03

Astronomy and Astrophysics

Astrophysics

Scientific paper

We have investigated three-body effect for p(pe^-, ν_e)d reaction in nuclear astrophysics. Solutions of three-body equation for the initial pep state show that two-proton dynamics does not depend on the electron degrees of freedom and hence the conventional adiabatic approximation is valid for energy sector (E_ep/E_pp) > 10-3 where E_ep and E_pp are the relative kinetic energies between e and p, and between p and p, respectively. For the energy sector (E_ep/E_pp) ≈ 10-3, an exact solution of the three-body equation is required. For the energy sector (E_ep/E_pp) < 10-3, it is shown that a Gamow-factor cancellation (GFC) can occur between two protons. Our estimate of the GFC effect indicates that the previous conventional estimate of the pep solar neutrino flux may be an underestimate at least by a factor of two. Implications of our results for the solar neutrino problem are described. At lower temperatures, the GFC effect becomes more significant, and p(pe^-, ν_e)d may dominate over p(p,e^+ ν_e)d. The enhancement of the reaction rate for p(pe^-, νe )d at lower temperatures due to the GFC effect may offer possible explanations for some of long-standing anomalies in astrophysical and geophysical problems.

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