论文标题
在密度依赖性相对论平均模型中旋转中子星的特性
Properties of Rotating Neutron Star in Density-dependent Relativistic Mean-field Models
论文作者
论文摘要
开发了平衡序列，用于使用NS物质的四个密度依赖性状态方程在相对论平均场相互作用框架中旋转NS。这些序列是针对观察到的25、317、346、716和1122 Hz的旋转频率构建的。在每个模型中计算序列的边界以确定稳定性区域。计算重力质量，四极力矩，极性，前向和后向红移和Kerr参数。 DDF和DD-ME $δ$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 Hz的频率旋转。所有选定的EOSS均以716和1122 Hz的频率正确地描述了PSR J1748-244AD和PSR J1739-285的旋转。这些恒星的质量分别在[0.68，2.14] m $ _ {\ odot} $和[1.67，2.24] m $ _ {\ odot} $的范围内。在所有选定的旋转频率和开普勒序列中计算了极性，前后红移和四极力矩。结果与观察结果一致。确认$ 1.5^{+0.4} _ { - 1.0} m _ {\ odot} $的质量为Exo 0748-676，我们的结果将接近观察到的值，并且本研究中使用的eoss正确描述了这一星星。在所有型号中，Kerr参数，极性，向前和向后红移的极端都达到了a/m $ \ $ \ $ 0.7，z $ _ {p} \ $ $ 0.8，z $ _ {eq}^eq}^{f} {f} {f} {f} \ $ -0.3和z $ -0.3和z $ _ {eq}^a {eq}^$ 2.2。这些红移和Kerr参数的行为大致与EOS无关。观察到的行为必须通过其他EOSS进行评估，以找到这些数量的普遍关系。同样，每个参数中的每个参数都有一个极限值。在这种情况下，这些参数大于极限值，恒星可以以等于或大于$ν$ = 1122 Hz的频率旋转。
Equilibrium sequences were developed for rotating NS in the relativistic mean-field interaction framework using four density-dependent equations of state for the NS matter. These sequences were constructed for the observed rotation frequencies of 25, 317, 346, 716, and 1122 Hz. The bounds of 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. DDF and DD-ME$δ$ 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 Hz, respectively. All the selected EOSs properly described the rotation of PSR J1748-244ad, and PSR J1739-285 at a frequency of 716 and 1122 Hz, respectively. The mass of these stars was in the range of [0.68, 2.14]M$_{\odot}$ and [1.67, 2.24]M$_{\odot}$, respectively. The polar, forward and backward redshifts, and the quadrupole moment were calculated in all selected rotating frequencies and the Keplerian sequence. The results were consistent with observations. Confirming the mass of $1.5^{+0.4}_{-1.0}M_{\odot}$ for EXO 0748-676, our result will be close to the observed value, and the EOSs used in this study properly describe this star. The extremum of Kerr parameter, polar, forward and backward redshifts in all models reached constant values of, a/M$\approx$ 0.7, Z$_{p}\approx$ 0.8, Z$_{eq}^{f}\approx$ -0.3 and Z$_{eq}^{b}\approx$ 2.2. 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 $ν$= 1122 Hz.
