超临界带电体与正负电子对的产生
Supercritically charged objects and electron-positron pair creation
摘要：
本文在P-Fermi近似下研究了超临界荷电超重核、$ud$ QM核、奇异核和奇异子核的稳定性和$e^+e^-$对的产生。模型参数是固定的，通过复制他们的质量和电荷性质在早期出版物中报道。发现$ud$ QM块金、奇异子和奇异子块金可能分别在$A\gtrsim 315$、$5\times10^4$和$1.2\times10^8$处比${}^{56}$ Fe更稳定。对于那些对中子辐射稳定的元素，质量最大的超重元素的重子数为$\sim$ 965，而$ud$ QM块、奇异子和奇异子块的重子数需要大于$39$、433和$2.7\times10^5$。对于电荷数为$Z\geq177$的超重核、$Z\geq163$的$ud$ QM核、$Z\geq 192$的奇异核和$Z\geq 212$的奇异核，$e^+e^-$对的产生将不可避免地开始。在给定的电子化学势$\barμ_e$下，得到了一个普适关系式$Q/R_e = \left(m_e - \barμ_e\right)/α$，其中$Q$为总电荷，$R_e$为电子云半径.这通过取$\barμ_e=-m_e$来预测最大电荷数。对于含$\barμ_e<-m_e$的超临界带电体，基于JWKB近似，估算了$e^+e^-$对产生的衰变率。发现大多数正电子发射在$t\lesssim 10^{-15}$ s，而一个持久的正电子发射观察到大对象与$R\gtrsim 1000$ fm。超临界带电天体的正电子发射和湮灭可能是导致致密双星合并过程中短$γ$射线爆发、511 keV连续辐射以及星系和星系团X射线谱中窄的微弱发射线的部分原因。
英文摘要：
We investigate the stability and $e^+e^-$ pair creation of supercritically charged superheavy nuclei, $ud$QM nuggets, strangelets, and strangeon nuggets based on Thomas-Fermi approximation. The model parameters are fixed by reproducing their masses and charge properties reported in earlier publications. It is found that $ud$QM nuggets, strangelets, and strangeon nuggets may be more stable than ${}^{56}$Fe at $A\gtrsim 315$, $5\times10^4$, and $1.2\times10^8$, respectively. For those stable against neutron emission, the most massive superheavy element has a baryon number $\sim$965, while $ud$QM nuggets, strangelets, and strangeon nuggets need to have baryon numbers larger than $39$, 433, and $2.7\times10^5$. The $e^+e^-$ pair creation will inevitably start for superheavy nuclei with charge numbers $Z\geq177$, $ud$QM nuggets with $Z\geq163$, strangelets with $Z\geq 192$, and strangeon nuggets with $Z\geq 212$. A universal relation $Q/R_e = \left(m_e - \barμ_e\right)/α$ is obtained at a given electron chemical potential $\barμ_e$, where $Q$ is the total charge and $R_e$ the radius of electron cloud. This predicts the maximum charge number by taking $\barμ_e=-m_e$. For supercritically charged objects with $\barμ_e<-m_e$, the decay rate for $e^+e^-$ pair production is estimated based on the JWKB approximation. It is found that most positrons are emitted at $t\lesssim 10^{-15}$ s, while a long lasting positron emission is observed for large objects with $R\gtrsim 1000$ fm. The emission and annihilation of positrons from supercritically charged objects may be partially responsible for the short $γ$-ray burst during the merger of binary compact stars, the 511 keV continuum emission, as well as the narrow faint emission lines in X-ray spectra from galaxies and galaxy clusters.
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