具有大部分地壳转动惯量的船帆座脉冲星的二分量模型
A Two Component Model of the Vela Pulsars with Large Fractional Moment of Inertia of the Crust
摘要：
我们构造了船帆座脉冲星的二分量分析模型，它能再现质量范围为$M/M_\odot \geq 1.0 - 1.96$的部分地壳转动惯量$I_{\rm crust}/I_{\rm total} \geq 0.074$（其中$I_{\rm crust}$表示地壳转动惯量，$ I_{\rm total}$是恒星的总转动惯量）。模型假定在表面密度$E_a = 2\times 10^{14}\rm g{cm}^{-3}$（如Brecher和Caporaso的\cite{Ref1}）处是自约束的，这产生了核壳边界处的过渡密度$E_b \geq 2.105 \times 10^{14}\rm g{cm}^{-3}$和压力/能量密度比$P_b/E_b \geq 0.00589$。模型的中心密度$E_0$的范围为1.263 - 1.600 $\times 10^{15}\rm g{cm}^{-3}$。总转动惯量$I_{\rm total}$和地壳成分的转动惯量$ I_{\rm crust}$分别在$I_{\rm 45} = $ 0.076 - 2.460和0.0056 - 0.8622的范围内（其中$I_{45}=I/10^{45}\rm g{cm}^2$ .模型的总半径$a$为9.252 - 11.578km，地壳厚度$a_{\rm crust}$为0.234 - 1.551km。模型的地壳质量$M_{\rm crust}/M_\odot$在0.025 - 0.263之间变化。压力/能量密度比，$P_b/E_b$，在核壳边界和其他物理参数在这项研究中获得的船帆座脉冲星与文献中获得的相应参数的基础上的各种状态方程（EOSs）进行了比较。在文献\cite{Ref2}、\cite{Ref3}中，很少有研究预测船帆座质量为1.7 $M_\odot$时的分数地壳转动惯量约为7%，本研究能够重现船帆座脉冲星在1.0 - 1.96 $M\odot$范围内所有质量值的最小分数地壳惯性转动惯量约为7.4%和更大。
英文摘要：
We construct a two-component analytic model of the Vela pulsar which can reproduce the fractional crustal moment of inertia, $I_{\rm crust}/I_{\rm total} \geq 0.074$ ( where $I_{\rm crust}$ represents the moment of inertia of the crust and $ I_{\rm total}$ is the total moment of inertia of the star) for the mass range $M/M_\odot \geq 1.0 - 1.96$. The models are assumed to be self-bound at the surface density $E_a = 2\times 10^{14}\rm g{cm}^{-3}$ (like, Brecher and Caporaso \cite{Ref1}) which yields the transition density at the core-crust boundary $E_b \geq 2.105 \times 10^{14}\rm g{cm}^{-3}$ and pressure/energy-density ratio, $P_b/E_b \geq 0.00589$.The central density, $E_0$, of the models ranges from 1.263 - 1.600 $\times 10^{15}\rm g{cm}^{-3}$. The total moment of inertia, $I_{\rm total}$, and the moment of inertia of the crust component, $ I_{\rm crust}$ lie in the range $I_{\rm 45} = $0.076 - 2.460 and 0.0056 - 0.8622 respectively (where $I_{45}=I/10^{45}\rm g{cm}^2$. The total radii, $a$, of the models have the values from 9.252km - 11.578km and the crustal thickness, $a_{\rm crust}$, lies in the range 0.234km - 1.551km. The mass of the crust, $M_{\rm crust}/M_\odot$, of the models varies from 0.025 - 0.263. The pressure/energy-density ratio, $P_b/E_b$, at the core-crust boundary and other physical parameters obtained in this study for the Vela pulsar are compared with the corresponding parameters obtained in the literature on the basis of various equations of state (EOSs). That few studies available in the literature \cite{Ref2}, \cite{Ref3} which predict the fractional crustal moment of inertia about 7\% for the Vela mass as large as 1.7$M_\odot$, the present study has been able to reproduce the minimum fractional crustal moment of inertia about 7.4\% and larger for all the values of the mass in the range 1.0 - 1.96$M\odot$ considered for the Vela pulsar.
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