船帆座脉冲星的核包层解析模型
A Core-envelope Analytic Model for the Vela Pulsar
摘要：
本文研究了{Ref 1}、{Ref 2}中提出的实芯-包络模型，它们对应于致密性参数$u \equiv M/a$ = 0.30和0.25（几何单位的质量与尺寸比）。可以看出，这些模型能够解释船帆座脉冲星的毛刺愈合参数$G_h = I_{\rm core}/I_{\rm total} < 0.55$ {Ref 3}的所有观测值。对于船帆座脉冲星，在$M = 3.079M_\odot - 2.263M_\odot$、$z_a = 0.581 - 0.414$和$I_{\rm Vela,45} =6.9 - 3.5$（其中$I_{45}=I/10^{45}\rm g{cm}^2$）范围内，模型分别给出了质量$M$、表面红移$z_a$和转动惯量$I_{\rm Vela}$的最大值，$u = $值为0.30和0.25，表面密度指定值为$E_a = 2\times 10^{14}\rm g{cm}^{-3}$ {Ref 4}。质量值低于上述值（所谓的实际质量范围，$M = 1.4\pm0.2 M_\odot$，但显著高于不切实际的质量范围$M \leq 0.5M_\odot$（在文献中根据致密核物质状态方程（EOSs）的参数化中子星（NS）模型获得船帆座脉冲星{Ref 3}）并且对于对应于$u < 0.25$值的上述$G_h$值的范围，同样可以获得其它参数。模型被发现是因果一致的，引力约束和脉动稳定。实际上，本研究中得到的中子星（NS）质量上界（适用于船帆座脉冲星）对应于经典结果{Ref 5}和基于现代中子星物质的EOS得到的NS质量上界的平均值{Ref 6}，并且与最新的理论估计{Ref 7}一致。
英文摘要：
The core-envelope models presented in {Ref1}; {Ref2}, corresponding to the values of compactness parameter, $u \equiv M/a$ = 0.30 and 0.25 (mass to size ratio in geometrized units) have been studied under slow rotation. It is seen that these models are capable of explaining all the observational values of glitch healing parameter, $G_h = I_{\rm core}/I_{\rm total} < 0.55$ {Ref3} for the Vela pulsar. The models yield the maximum values of mass, $M$, surface redshift, $z_a$, and the moment of inertia, $I_{\rm Vela}$ for the Vela pulsar in the range $M = 3.079M_\odot - 2.263M_\odot$; $z_a = 0.581 - 0.414$ and $I_{\rm Vela,45} =6.9 - 3.5$ (where $I_{45}=I/10^{45}\rm g{cm}^2$) respectively for the values of $u = $ 0.30 and 0.25 and for an assigned value of the surface density, $E_a = 2\times 10^{14}\rm g{cm}^{-3}$ {Ref4}. The values of masses lower than the above mentioned values ( so called the realistic mass range, $M = 1.4\pm0.2 M_\odot$, in the literature) but significantly higher than that of the unrealistic mass range $M \leq 0.5M_\odot$ (obtained for the Vela pulsar in the literature on the basis of parametrized neutron star (NS) models based on equations of state (EOSs) of dense nuclear matter {Ref3}) and other parameters may be obtained likewise for the above mentioned range of the values of $G_h$ corresponding to the values of $u < 0.25$. The models are found to be causally consistent, gravitational bound and pulsationally stable. The upper bound on neutron star (NS) mass obtained in this study which is applicable for the Vela pulsar, in fact, corresponds to the mean value of the upper bound on NS mass obtained in the classical result {Ref5} and that obtained on the basis of modern EOSs for neutron star matter {Ref6} and is in a good agreement with the most recent theoretical estimate {Ref7}.
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