The nuclear physics input from the 3He(a,g)7Be cross section is a major uncertainty in the fluxes of 7Be and 8B neutrinos from the Sun predicted by solar models and in the 7Li abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt- technique and with inferior precision. Using a windowless gas target, high beam intensity and low background g-counting facilities, the 3He(a,g)7Be cross section has been determined at 127, 148 and 169 keV center-of-mass energy with a total uncertainty of 4%. The sources of systematic uncertainty are discussed in detail. The present data can be used in big-bang nucleosynthesis calculations and to constrain the extrapolation of the 3He(a,g)7Be astrophysical S-factor to solar energies.

The nuclear physics input from the He3(α,γ)Be7 cross section is a major uncertainty in the fluxes of Be7 and B8 neutrinos from the Sun predicted by solar models and in the Li7 abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt-γ technique and with inferior precision. Using a windowless gas target, high beam intensity, and low background γ-counting facilities, the He3(α,γ)Be7 cross section has been determined at 127, 148, and 169 keV center-of-mass energy with a total uncertainty of 4%. The sources of systematic uncertainty are discussed in detail. The present data can be used in big-bang nucleosynthesis calculations and to constrain the extrapolation of the He3(α,γ)Be7 astrophysical S factor to solar energies. © 2006 The American Physical Society.

Activation measurement of the 3He(alfa,gamma )7Be cross section at low energy

COSTANTINI, HEIDE;CORVISIERO, PIETRO;LEMUT, ALBERTO;PRATI, PAOLO;
2006-01-01

Abstract

The nuclear physics input from the He3(α,γ)Be7 cross section is a major uncertainty in the fluxes of Be7 and B8 neutrinos from the Sun predicted by solar models and in the Li7 abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt-γ technique and with inferior precision. Using a windowless gas target, high beam intensity, and low background γ-counting facilities, the He3(α,γ)Be7 cross section has been determined at 127, 148, and 169 keV center-of-mass energy with a total uncertainty of 4%. The sources of systematic uncertainty are discussed in detail. The present data can be used in big-bang nucleosynthesis calculations and to constrain the extrapolation of the He3(α,γ)Be7 astrophysical S factor to solar energies. © 2006 The American Physical Society.
2006
The nuclear physics input from the 3He(a,g)7Be cross section is a major uncertainty in the fluxes of 7Be and 8B neutrinos from the Sun predicted by solar models and in the 7Li abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt- technique and with inferior precision. Using a windowless gas target, high beam intensity and low background g-counting facilities, the 3He(a,g)7Be cross section has been determined at 127, 148 and 169 keV center-of-mass energy with a total uncertainty of 4%. The sources of systematic uncertainty are discussed in detail. The present data can be used in big-bang nucleosynthesis calculations and to constrain the extrapolation of the 3He(a,g)7Be astrophysical S-factor to solar energies.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11567/227597
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