标题： 各向异性夸克星在全广义相对论中的准正则f模 显示英文标题

标题： Quasi-normal f-modes of anisotropic quark stars in full general relativity

摘要： 我们研究了各向异性夸克星的f模振荡，在全广义相对论框架下。 我们考虑了两种不同的状态方程（EOS），一个是MIT袋模型EOS，另一个是EOS-A。 我们的研究检查了压力各向异性对平衡结构以及f模振荡频率和阻尼时间的影响。 我们的结果确认了f模频率与平均密度的平方根成线性关系，各向异性影响该关系的斜率和截距。 f模频率对总质量的依赖性揭示了基于切向压强和径向压强相对主导的不同趋势。 当切向压强超过径向压强时，频率随质量增加而增加，对于大质量夸克星表现出快速增长。 当径向压强占主导时，频率随质量增加而增加；然而，在径向压强明显大于切向压强的情况下，频率随质量增加而减少。 对于低质量夸克星，更强的切向压强会导致频率增加，而在某个临界质量以上，切向压强的进一步增加会导致频率减少。 对于所选择的各向异性强度范围，MIT袋模型EOS的频率在1.3 kHz到2.3 kHz之间，而EOS-A的频率在1.8 kHz到3.4 kHz之间。 我们发现归一化的阻尼时间与致密性呈线性关系。 对于固定的恒星质量，相对于径向压强，切向压强的增加会减少阻尼时间，而切向压强的减少则会显著增加它。 MIT袋模型EOS的阻尼时间范围为83毫秒到900毫秒，而EOS-A的阻尼时间范围为60毫秒到761毫秒。 我们提出了频率和阻尼时间作为质量、半径和各向异性强度函数的半经验表达式。 显示英文摘要

摘要： We investigate f-mode oscillations of anisotropic quark stars within the framework of full general relativity. We consider two different equations of state (EOSs), one is the MIT bag model EOS and the other is EOS-A. Our study examines the impact of the pressure anisotropy on the equilibrium structure, as well as on the frequencies and damping times of f-mode oscillations. Our results confirm that the f-mode frequency scales linearly with the square root of the average density, with anisotropy influencing both the slope and intercept of this relation. The dependence of the f-mode frequency on total mass reveals distinct trends based on the relative dominance of tangential and radial pressure. When the tangential pressure exceeds the radial pressure, the frequency increases with mass, exhibiting rapid growth for massive quark stars. When the radial pressure dominates, the frequency increases with mass; however, in cases where the radial pressure is significantly greater than the tangential pressure, the frequency decreases as mass increases. For low-mass quark stars, stronger tangential pressure leads to an increase in frequency, while beyond a threshold mass, a further increase in tangential pressure results in a decrease in frequency. For the chosen range of anisotropic strengths, the frequency varies between 1.3 kHz and 2.3 kHz for the MIT bag EOS and between 1.8 kHz and 3.4 kHz for EOS-A. We find that the normalized damping time follows a linear trend with compactness. For a fixed stellar mass, an increase in tangential pressure relative to radial pressure reduces the damping time, whereas a decrease in tangential pressure significantly increases it. The damping time ranges from 83 ms to 900 ms for the MIT bag EOS and from 60 ms to 761 ms for EOS-A. We present semi-empirical expressions for both the frequency and damping time as functions of mass, radius, and anisotropic strength.