Astrophysical <I>S</I>-factor of the d(p,γ)<SUP>3</SUP>He processby

H. Sadeghi; H. Khalili; M. Godarzi

doi:10.1088/1674-1137/37/4/044102

Chinese Physics C> 2013, Vol. 37> Issue(4) : 044102 DOI: 10.1088/1674-1137/37/4/044102

Astrophysical S-factor of the d(p,γ)³He processby

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Abstract：
We summarize the recent effective field theory (EFT) studies of low-energy electroweak reactions of astrophysical interest, relevant to big-bang nucleosynthesis. The zero energy astrophysical S(0) factor for the thermal proton radiative capture by deuteron is calculated with pionless EFT. The astrophysical S(0) factor is accurately determined to be S(0)=0.243 eV·b up to the leading order (LO). At zero energies, magnetic transition M₁ gives the dominant contribution. The M₁ amplitude is calculated up to the LO. A good, quantitative agreement between theoretical and experimental results is found for all observables. The demonstrations of cutoff independent calculation have also been presented.

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H. Sadeghi, H. Khalili and M. Godarzi. Astrophysical S-factor of the d(p,γ)³He processby[J]. Chinese Physics C, 2013, 37(4): 044102. doi: 10.1088/1674-1137/37/4/044102

H. Sadeghi, H. Khalili and M. Godarzi. Astrophysical S-factor of the d(p,γ)³He processby[J]. Chinese Physics C, 2013, 37(4): 044102. doi: 10.1088/1674-1137/37/4/044102 shu

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Received: 2012-05-21
Revised: 1900-01-01

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通讯作者: 陈斌, bchen63@163.com

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沈阳化工大学材料科学与工程学院沈阳 110142

Astrophysical S-factor of the d(p,γ)³He processby

Corresponding author: H. Sadeghi,

Received Date: 2012-05-21

Accepted Date: 1900-01-01

Available Online: 2013-04-05

Abstract: We summarize the recent effective field theory (EFT) studies of low-energy electroweak reactions of astrophysical interest, relevant to big-bang nucleosynthesis. The zero energy astrophysical S(0) factor for the thermal proton radiative capture by deuteron is calculated with pionless EFT. The astrophysical S(0) factor is accurately determined to be S(0)=0.243 eV·b up to the leading order (LO). At zero energies, magnetic transition M₁ gives the dominant contribution. The M₁ amplitude is calculated up to the LO. A good, quantitative agreement between theoretical and experimental results is found for all observables. The demonstrations of cutoff independent calculation have also been presented.

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Astrophysical S-factor of the d(p,γ)3He processby

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Astrophysical S-factor of the d(p,γ)³He processby

Astrophysical S-factor of the d(p,γ)³He processby