$^{206}$ Pb中的俾格米和核心极化偶极模：将原子核结构与恒星核合成联系起来
Pygmy and core polarization dipole modes in $^{206}$Pb: connecting nuclear structure to stellar nucleosynthesis
摘要：
使用HI $\vecγ$ S设施的（$\vecγ$，$γ'$）实验对低于中子分离能的$^{206}$ Pb的电磁响应进行高分辨率研究。用100%线偏振光子束的核共振荧光测量了$^{206}$ Pb从$4.9$到$8.1$ MeV激发态的自旋、宇称、分支比和衰变宽度。对于低于中子分离能的总电偶极和磁偶极强度，提取的$Σ$ $B$（E1）$\uparrow$和$Σ$ $B$（M1）$\uparrow$值分别为0.9 $\pm$ 0.2 e $^2$ fm $^2$和8.3 $\pm$ 2.0 $μ_{N}^2$。这些测量被发现是在非常好的协议与预测从能量密度泛函（EDF）加准粒子声子模型（QPM）。这样一个详细的理论分析，可以分开的巨偶极共振和多声子激发的尾巴的侏儒偶极共振。结合早期的光核实验以上的中子分离能，提取的值为$α_{D}\!=\!122\pm10$ mb/MeV的$^{206}$铅的电偶极极化率。当与EDF+QPM和精确校准的相对论EDF的预测相比较时，可以推导出$R_{\rm skin}^{206}\!=\!0.12$ - $0.19$ fm的中子皮厚度范围和$L\!=\!48$ - $60$ MeV的对称能斜率的相应范围。这个新获得的信息也被用来估计麦克斯韦平均辐射截面$^{205}$ Pb（n，$γ$）$^{206}$ Pb在30 keV是$σ\!=\!130\!\pm\!25$ mb。这种测量的天体物理学的影响-在恒星核合成的S-过程和状态方程的中子丰富的物质-进行了讨论。
英文摘要：
A high-resolution study of the electromagnetic response of $^{206}$Pb below the neutron separation energy is performed using a ($\vecγ$,$γ'$) experiment at the HI$\vecγ$S facility. Nuclear resonance fluorescence with 100% linearly polarized photon beams is used to measure spins, parities, branching ratios, and decay widths of excited states in $^{206}$Pb from $4.9$ to $8.1$MeV. The extracted $Σ$$B$(E1)$\uparrow$ and $Σ$$B$(M1)$\uparrow$ values for the total electric and magnetic dipole strength below the neutron separation energy are 0.9$\pm$0.2e$^2$fm$^2$ and 8.3$\pm$2.0$μ_{N}^2$, respectively. These measurements are found to be in very good agreement with the predictions from an energy-density functional (EDF) plus quasiparticle phonon model (QPM). Such a detailed theoretical analysis allows to separate the pygmy dipole resonance from both the tail of the giant dipole resonance and multi-phonon excitations. Combined with earlier photonuclear experiments above the neutron separation energy, one extracts a value for the electric dipole polarizability of $^{206}$Pb of $α_{D}\!=\!122\pm10$mb/MeV. When compared to predictions from both the EDF+QPM and accurately calibrated relativistic EDFs, one deduces a range for the neutron-skin thickness of $R_{\rm skin}^{206}\!=\!0.12$-$0.19$fm and a corresponding range for the slope of the symmetry energy of $L\!=\!48$-$60$MeV. This newly obtained information is also used to estimate the Maxwellian-averaged radiative cross section $^{205}$Pb(n,$γ$)$^{206}$Pb at 30keV to be $σ\!=\!130\!\pm\!25$mb. The astrophysical impact of this measurement--on both the s-process in stellar nucleosynthesis and on the equation of state of neutron-rich matter--is discussed.
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