论文标题
$λnn$含量$λ$ -Nucleus潜力的$λ$ hypernuclei的约束
Constraints from $Λ$ hypernuclei on the $ΛNN$ content of the $Λ$-nucleus potential
论文作者
论文摘要
1988年通过研究$λ$ -Nucleus电位的$d_λ\约-28 $ MEV的深度通过研究从元素周期表中测得的$（π^+，k^+）$ spectra推导的$λ$ binding engies来确认。现代的两体超声核子交互模型需要附加的交互项，很可能是$λnn$三体术语，以复制$d_λ$。在这项工作中，我们应用了适当构建的$λ$ -Nucleus密度相关的光学潜力，以结合观察到的$1S_λ$和$1P_λ$状态的能量计算，$ 12 \ leq a \ leq a \ leq leq 208 $。产生的$λnn$贡献了$d_λ$，在对称的核物质密度$ρ_0= 0.17 $ fm $^{ - 3} $时，大约14 mev copulsion $d_λ$在$ρ\ gtrsim3ρ_0$中使$d_λ$越来越令人反感。这表明在某些模型中，状态僵硬的方程式可能支持两个太阳质量中子星。
A depth of $D_Λ\approx -28$ MeV for the $Λ$-nucleus potential was confirmed in 1988 by studying $Λ$ binding energies deduced from $(π^+,K^+)$ spectra measured across the periodic table. Modern two-body hyperon-nucleon interaction models require additional interaction terms, most likely $ΛNN$ three-body terms, to reproduce $D_Λ$. In this work we apply a suitably constructed $Λ$-nucleus density dependent optical potential to binding energy calculations of observed $1s_Λ$ and $1p_Λ$ states in the mass range $12\leq A\leq 208$. The resulting $ΛNN$ contribution to $D_Λ$, about 14 MeV repulsion at symmetric nuclear matter density $ρ_0=0.17$ fm$^{-3}$, makes $D_Λ$ increasingly repulsive at $ρ\gtrsim 3ρ_0$, leading possibly to little or no $Λ$ hyperon content of neutron-star matter. This suggests in some models a stiff equation of state that may support two solar-mass neutron stars.
