Equilibrium sequences were developed for rotating neutron stars in the relativistic mean-field interaction framework using four density-dependent equations of state (EOSs) for the neutron star matter. These sequences were constructed for the observed rotation frequencies of 25, 317, 346, 716 and 1122[Formula: see text]Hz. The bounds of sequences, the secular axisymmetric instability, static and Keplerian sequences were calculated in each model to determine the stability region. The gravitational mass, quadrupole moment, polar, forward and backward redshifts, and Kerr parameter were calculated according to this stability region, and the allowable range of these quantities was then determined for each model. According to the results, DDF and DD-ME[Formula: see text] were unable to properly describe the low-frequency neutron stars, PSR J0348+432, PSR J1614-2230 and PSR J0740+6620 rotate at a frequency of 25, 317 and 346[Formula: see text]Hz, respectively. On the other hand, all the selected EOSs properly described the rotation of PSR J1748-244ad and PSR J1739-285 at a frequency of 716 and 1122[Formula: see text]Hz, respectively. The mass of these stars was, therefore, in the range of [Formula: see text] and [Formula: see text], respectively. The polar, forward and backward redshifts, and the quadrupole moment were calculated in all the selected rotating frequencies and the Keplerian sequence. The results were consistent with observations. Confirming the mass of [Formula: see text] for EXO 0748-676, our result, [Formula: see text], will be close to the observed value, and the EOSs used in this study properly describe this star. Interestingly, the extremum of Kerr parameter, polar, forward and backward redshifts in all models reached constant values of, [Formula: see text], [Formula: see text], [Formula: see text] and [Formula: see text], respectively. These behaviors of redshifts and Kerr parameter are approximately independent of EOS. The observed behaviors must evaluate by other EOSs to find universal relations for these quantities. Also, a limit value was found for each of these parameters. In this case where these parameters are greater than the limit value, the star can rotate at a frequency equal to or greater than [Formula: see text][Formula: see text]Hz.

中文翻译：

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密度相关的相对论平均场模型中旋转中子星的性质

使用中子星物质的四个密度相关状态方程 (EOS)，在相对论平均场相互作用框架中为旋转中子星开发了平衡序列。这些序列是针对观察到的 25、317、346、716 和 1122 [公式：见文本]Hz 的旋转频率构建的。在每个模型中计算序列的边界、长期轴对称不稳定性、静态和开普勒序列以确定稳定区域。引力质量、四极矩、极性、前向和后向红移和克尔参数都是根据这个稳定区域计算出来的，然后确定每个模型的这些量的允许范围。根据结果​​，DDF和DD-ME[公式：见正文]无法正确描述低频中子星PSR J0348+432，PSR J1614-2230 和 PSR J0740+6620 分别以 25、317 和 346[公式：见正文]Hz 的频率旋转。另一方面，所有选定的 EOS 都正确地描述了 PSR J1748-244ad 和 PSR J1739-285 分别以 716 和 1122[公式：见正文]Hz 的频率旋转。因此，这些恒星的质量分别在[公式：见正文]和[公式：见正文]的范围内。在所有选定的旋转频率和开普勒序列中计算了极坐标、前向和后向红移以及四极矩。结果与观察结果一致。确认 EXO 0748-676 的 [公式：见文本] 的质量，我们的结果 [公式：见文本] 将接近观测值，并且本研究中使用的 EOS 正确地描述了这颗恒星。有趣的是，克尔参数的极值极值，所有模型中的正向和反向红移分别达到[公式：见文本]、[公式：见文本]、[公式：见文本]和[公式：见文本]的恒定值。这些红移行为和 Kerr 参数几乎与 EOS 无关。观察到的行为必须由其他 EOS 评估，以找到这些量的普遍关系。此外，还为这些参数中的每一个找到了一个极限值。在这些参数大于极限值的情况下，恒星可以以等于或大于[公式：见文本][公式：见文本]Hz的频率旋转。观察到的行为必须由其他 EOS 评估，以找到这些量的普遍关系。此外，还为这些参数中的每一个找到了一个极限值。在这些参数大于极限值的情况下，恒星可以以等于或大于[公式：见文本][公式：见文本]Hz的频率旋转。观察到的行为必须由其他 EOS 评估，以找到这些量的普遍关系。此外，还为这些参数中的每一个找到了一个极限值。在这些参数大于极限值的情况下，恒星可以以等于或大于[公式：见文本][公式：见文本]Hz的频率旋转。