标题： 质子-氘辐射俘获的大爆炸核合成 implications 显示英文标题

标题： Implication of the proton-deuteron radiative capture for Big Bang Nucleosynthesis

摘要： The astrophysical $S$-factor for the radiative capture $d(p,\gamma)^3$He in the energy-range of interest for Big Bang Nucleosynthesis (BBN) is calculated using an {\it 从头计算} approach. The nuclear Hamiltonian retains both two- and three-nucleon interactions - the Argonne $v_{18}$ and the Urbana IX, respectively. Both one- and many-body contributions to the nuclear current operator are included. The former retain for the first time, besides the $1/m$ leading order contribution ($m$ is the nucleon mass), also the next-to-leading order term, proportional to $1/m^3$. The many-body currents are constructed in order to satisfy the current conservation relation with the adopted Hamiltonian model. 超球谐波技术被应用于求解$A=3$的束缚态和散射态。在第二种情况下，特别注意以获得大爆炸核合成（BBN）能量范围内的不确定性，使得天体物理$S$因子的不确定度达到或低于$\sim$的 1%。然后，在这个能量范围内，发现$S$因子比目前采用的值高$\sim$10%。其中一部分增加（1-3%）归因于单体算符$1/m^3$，而其余部分则归因于新的更精确的散射波函数。 我们研究了这一新测定对氘 primordial 丰度的$d(p,\gamma)^3$氦$S$因子的影响。我们发现，使用普朗克实验最近测定的重子密度以及在原初核合成期间标准的相对论自由度数$N_{\rm eff}=3.046$的情况下，预测的$^2$氢丰度比理论值与其实验测定结果非常一致。 显示英文摘要

摘要： The astrophysical $S$-factor for the radiative capture $d(p,\gamma)^3$He in the energy-range of interest for Big Bang Nucleosynthesis (BBN) is calculated using an {\it ab-initio} approach. The nuclear Hamiltonian retains both two- and three-nucleon interactions - the Argonne $v_{18}$ and the Urbana IX, respectively. Both one- and many-body contributions to the nuclear current operator are included. The former retain for the first time, besides the $1/m$ leading order contribution ($m$ is the nucleon mass), also the next-to-leading order term, proportional to $1/m^3$. The many-body currents are constructed in order to satisfy the current conservation relation with the adopted Hamiltonian model. The hyperspherical harmonics technique is applied to solve the $A=3$ bound and scattering states. A particular attention is used in this second case in order to obtain, in the energy range of BBN, an uncertainty on the astrophysical $S$-factor of the order or below $\sim$1 %. Then, in this energy range, the $S$-factor is found to be $\sim$10 % larger than the currently adopted values.Part of this increase (1-3 %) is due to the $1/m^3$ one-body operator, while the remaining is due to the new more accurate scattering wave functions. We have studied the implication of this new determination for the $d(p,\gamma)^3$He $S$-factor on deuterium primordial abundance. We find that the predicted theoretical value for $^2$H/H is in excellent agreement with its experimental determination, using the most recent determination of baryon density of Planck experiment, and with a standard number of relativistic degrees of freedom $N_{\rm eff}=3.046$ during primordial nucleosynthesis.