Physics of the Dark Universe最新文献_第5页

Interior structure and physical features of dark energy relativistic stars in power law gravity model 幂律引力模型中暗能量相对论恒星的内部结构和物理特征

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-25 DOI: 10.1016/j.dark.2025.102198

M.R. Shahzad , Wajiha Habib , Asifa Ashraf , Muneerah Alomar , Awatef Abidi , Maryam Al Huwayz

The modeling of astrophysical compact objects has recently attracted significant interest of the research community to understand their stable internal structures. In particular, the addition of dark energy as another source of matter configuration in the interiors of such stars has elevated the focus on their theoretical development. In this study, we present a ne model of static, spherically symmetric, and anisotropic compact stars within the framework of f(R) modified theories. The stellar structure is described by a two-fluid system consisting of ordinary matter and dark energy. We develop the analytical solutions to the governing modified field equations using the well-known Finch-Skea ansatz for the metric potentials, coupled with a linear equation of state for the dark energy component. The model parameters, including the metric ansatz, are determined via smooth matching conditions at the boundary between the interior and exterior spacetime regions. To demonstrate the physical viability of the model, we apply our formulation to the compact star 4U 1538-52, utilizing the stable and widely studied

f (R) = R + 2 χ R^{2}

gravity model. We analyze an extensive investigation of the physical features, including the behavior of metric equations, matter variables, energy conditions, and stability criteria. In addition, we evaluate the evolution of the mass function, surface redshift, and compactness factor of the considered compact star candidates. The results confirm the stability, feasibility, and physical impact of the constructed solutions along with presenting additional insight into the interplay between dark energy structures and modified gravity within astrophysical circumstances. Graphical representations of key parameters enhance the clarity of our findings. The results demonstrate that our model is physically acceptable and stable in f(R) gravity.

天体物理致密物体的建模最近引起了研究界的极大兴趣，以了解它们稳定的内部结构。特别是，暗能量作为这类恒星内部物质结构的另一个来源的增加，提高了对它们理论发展的关注。在这项研究中，我们提出了一个在f(R)修正理论框架内的静态、球对称和各向异性致密恒星的新模型。恒星结构被描述为由普通物质和暗能量组成的双流体系统。我们利用著名的芬奇-斯基方差分析得到了控制修正场方程的解析解，并结合了暗能量分量的线性状态方程。模型参数，包括度量参数，通过内外时空区域边界的平滑匹配条件确定。为了证明该模型的物理可行性，我们利用稳定且广泛研究的f(R)=R+2χR2重力模型，将我们的公式应用于紧凑恒星4U 1538-52。我们分析了物理特征的广泛调查，包括度量方程的行为，物质变量，能量条件和稳定性标准。此外，我们评估了被考虑的紧致恒星候选者的质量函数、表面红移和紧致系数的演变。结果证实了构建的解决方案的稳定性、可行性和物理影响，同时对暗能量结构和天体物理环境下修正引力之间的相互作用提供了额外的见解。关键参数的图形表示增强了我们研究结果的清晰度。结果表明，该模型在f(R)重力下是物理上可接受的和稳定的。

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引用次数: 0

Quantum corrections and exotic criticality in charged rotating BTZ black holes 带电旋转BTZ黑洞中的量子修正和奇异临界

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-24 DOI: 10.1016/j.dark.2025.102202

Erdem Sucu, İzzet Sakallı

We investigate quantum corrections to the thermodynamics of charged, rotating BTZ black holes in AdS spacetime using both Generalized Uncertainty Principle (GUP) and exponential entropy corrections. The Hamilton–Jacobi tunneling method yields the Hawking temperature and its GUP-modified form, revealing how Planck-scale effects suppress thermal radiation. Exponential corrections to the Bekenstein-Hawking entropy lead to modified expressions for internal energy, Helmholtz and Gibbs free energies, pressure, enthalpy, and heat capacity. The AdS radius ℓ emerges as a critical parameter: smaller values enhance gravitational confinement and thermodynamic stability, while larger values weaken these effects. The heat capacity remains positive across parameter space, ruling out second-order phase transitions. However, the JT coefficient exhibits remarkable oscillatory behavior near r_h ≈ 1.05, alternating between heating and cooling phases during isenthalpic expansion. These oscillations intensify with increasing ℓ, indicating reduced stability in weakly curved AdS backgrounds. Gravitational redshift calculations in the weak-field limit show that the logarithmic charge coupling produces unbounded growth at large distances, with strong ℓ-dependence providing observational signatures. Our results demonstrate that (2+1)-dimensional black holes possess richer thermodynamic structure than their higher-dimensional counterparts, with quantum corrections introducing novel critical phenomena while preserving overall stability. These findings connect microscopic quantum gravity effects to macroscopic thermodynamic behavior, offering new perspectives on black hole physics in lower dimensions.

我们利用广义不确定性原理（GUP）和指数熵修正研究了AdS时空中带电旋转BTZ黑洞热力学的量子修正。Hamilton-Jacobi隧穿法产生了霍金温度及其修正后的gup形式，揭示了普朗克尺度效应是如何抑制热辐射的。对贝肯斯坦-霍金熵的指数修正导致了内能、亥姆霍兹和吉布斯自由能、压力、焓和热容的修正表达式。AdS半径作为一个关键参数出现：较小的值增强了引力约束和热力学稳定性，而较大的值则减弱了这些影响。热容在参数空间上保持正值，排除了二阶相变。然而，JT系数在rh ≈ 1.05附近表现出显著的振荡行为，在等焓膨胀过程中在加热阶段和冷却阶段之间交替。这些振荡随着r的增加而增强，表明弱弯曲AdS背景的稳定性降低。在弱场极限下的引力红移计算表明，对数电荷耦合在远距离上产生无界增长，具有强的依赖关系提供观测特征。我们的研究结果表明，（2+1）维黑洞比高维黑洞具有更丰富的热力学结构，量子修正在保持整体稳定性的同时引入了新的临界现象。这些发现将微观量子引力效应与宏观热力学行为联系起来，为较低维度的黑洞物理学提供了新的视角。

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引用次数: 0

Stability analysis and oscillatory behavior of orbits around Lorentz-violating black holes 违反洛伦兹黑洞轨道的稳定性分析和振荡行为

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-23 DOI: 10.1016/j.dark.2025.102200

Rana Muhammad Zulqarnain , Abdelmalek Bouzenada , Farruh Atamurotov , Ikhtiyor Saidov , A.S. Alqahtani , Phongpichit Channuie

In this paper, we investigate the motion of test particles around a black hole (BH) characterized by spontaneous Lorentz symmetry breaking, parameterized by α. We begin by outlining the theoretical framework underlying such BH geometries and subsequently analyze the corresponding dynamics of massive test particles. By applying the effective potential, we determine the exact conditions for circular trajectories and analyze the properties of the innermost stable circular orbits (ISCOs) parameters. In addition, the effective force acting on particles is studied, which gives further insight into orbital stability. Also, we are testing the BH shadow with M87* and Sgr A* under the influence of BH parameters.. Furthermore, we explore oscillatory phenomena associated with small perturbations around circular orbits, calculating the frequencies as measured by both local and distant observers, as well as the periastron precession. In this context, these results shed light on possible observational signatures of Lorentz-symmetry breaking in strong gravitational regimes and contribute to the understanding of modified BH physics.

本文研究了以自发洛伦兹对称破缺（α）为参数的黑洞周围测试粒子的运动。我们首先概述了这种黑洞几何形状的理论框架，随后分析了大质量测试粒子的相应动力学。利用有效势，我们确定了圆轨道的精确条件，并分析了最内层稳定圆轨道（ISCOs）参数的性质。此外，研究了作用在粒子上的有效作用力，对轨道稳定性有了进一步的认识。此外，我们还用M87*和Sgr A*在黑洞参数的影响下测试了黑洞阴影。此外，我们探索了与圆形轨道周围的小扰动相关的振荡现象，计算了由本地和远程观测者测量的频率，以及日冕进动。在这种背景下，这些结果揭示了在强引力条件下洛伦兹对称破缺的可能观测特征，并有助于理解修正的黑洞物理学。

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引用次数: 0

Novel solar system probes for primordial black holes 对原始黑洞的新型太阳系探测

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-21 DOI: 10.1016/j.dark.2025.102195

Oem Trivedi , Abraham Loeb

Primordial Black Holes (PBHs) represent one of the more interesting ways to address dark matter, at the interface of both cosmology and quantum gravity. It is no surprise then that testing PBHs is a venue of active interest, with several cosmological and astrophysical probes constraining different mass ranges. In this work, we propose novel Solar System scale searches for PBHs, motivated by the unique precision and coverage of local observables. We show that asteroid to dwarf planet mass PBHs can induce measurable dipolar timing signatures in pulsar timing arrays, while planetary mass PBHs can generate detectable ADAF accretion flares through interactions with Kuiper Belt bodies. Together, these complementary approaches open a new observational frontier for probing PBHs across mass ranges that remain unconstrained by conventional cosmological methods.

原始黑洞（PBHs）代表了一种更有趣的方式来解决暗物质，在宇宙学和量子引力的界面。毫无疑问，测试pbh是一个积极的兴趣点，有几个宇宙学和天体物理学探测器限制了不同的质量范围。在这项工作中，我们提出了新的太阳系尺度搜索pbh，动机是独特的精度和局部观测的覆盖范围。我们发现小行星到矮行星的质量pbh可以在脉冲星时序阵列中诱导可测量的偶极时序特征，而行星质量pbh可以通过与柯伊伯带天体的相互作用产生可检测的ADAF吸积耀斑。总之，这些互补的方法为探测不受传统宇宙学方法限制的质量范围内的pbh开辟了一个新的观测前沿。

引用次数: 0

Massive-photon electrodynamics and MHD in curved spacetime and cosmology 弯曲时空和宇宙学中的大质量光子电动力学和MHD

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-20 DOI: 10.1016/j.dark.2025.102192

Hyerim Noh , Jai-chan Hwang

We study a massive-photon electrodynamics and magnetohydrodynamics (MHD) in the curved spacetime of Einstein’s gravity. We consider a Proca-type photon mass and present equations in terms of electric and magnetic (EM) fields and the vector potential. We present the electrodynamics and MHD in the covariant and ADM formulations valid in general spacetime and in linearly perturbed cosmological spacetime. We present wave equations assuming the metric variations are negligible compared with the field variations. Equations are derived without fixing the temporal gauge condition and the gauge transformation properties of the EM fields and the vector potential are presented. Using the post-Newtonian approximation we show the dark Proca field behaves as dust in the non-relativistic limit under the Klein transformation.

研究了爱因斯坦引力下弯曲时空中的大质量光子电动力学和磁流体动力学。我们考虑了一个proca型光子质量，并给出了电磁场和矢量势的方程。我们提出了在一般时空和线性摄动宇宙学时空中有效的协变公式和ADM公式中的电动力学和MHD。我们提出波动方程，假设度规变化与场变化相比可以忽略不计。在不确定时间规范条件的情况下推导了方程，给出了电磁场和矢量势的规范变换性质。利用后牛顿近似，我们证明了在克莱因变换下的非相对论极限下，暗Proca场表现为尘埃。

引用次数: 0

Thermodynamic signatures of non-Abelian dilaton black holes 非阿贝尔膨胀黑洞的热力学特征

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-20 DOI: 10.1016/j.dark.2025.102197

Ankit Anand , Aditya Singh , Saeed Noori Gashti , Behnam Pourhassan

We investigate the thermodynamic extremality, topological charge structure, and thermodynamic curvature of non-Abelian dilaton black holes. The dilaton coupling significantly alters thermodynamic properties, enabling the verification of extremality conditions. By analyzing normalized thermodynamic vector fields, we classify topological charges through the identification of critical zero points, with their stability confirmed via winding number analysis. These topological sectors vary distinctly with the dilaton parameter. The free energy landscape is interpreted as a scalar field over parameter space, with its extrema corresponding to topological phases. This allows consistent charge assignments aligned with known solutions, such as the AdS Reissner-Nordström black hole. We further explore the topology of photon spheres and demonstrate their crucial role in black hole stability, establishing a strong link between thermodynamic topology and spacetime geometry. Finally, thermodynamic curvature is used to probe microscopic interactions, revealing predominantly attractive behavior with possible repulsive transitions near criticality. Our results indicate a rich phase structure and a non-trivial microstructure shaped by the interplay of dilaton and non-Abelian gauge fields.

研究了非阿贝尔膨胀黑洞的热力学极值性、拓扑电荷结构和热力学曲率。膨胀耦合显著地改变了热力学性质，使极端条件的验证成为可能。通过对归一化热力学向量场的分析，通过识别临界零点对拓扑电荷进行分类，并通过圈数分析确定拓扑电荷的稳定性。这些拓扑扇形随膨胀参数的变化而明显不同。自由能景观被解释为参数空间上的标量场，其极值对应于拓扑相。这使得电荷分配与已知的解决方案一致，例如AdS Reissner-Nordström黑洞。我们进一步探索了光子球的拓扑结构，并证明了它们在黑洞稳定性中的关键作用，建立了热力学拓扑和时空几何之间的紧密联系。最后，热力学曲率被用来探测微观相互作用，揭示了主要的吸引行为和可能的排斥转变接近临界。我们的结果表明，膨胀场和非阿贝尔规范场的相互作用形成了丰富的相结构和非平凡的微观结构。

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引用次数: 0

Is dark energy dynamical in the DESI era? A critical review 暗能量在DESI时代是动态的吗？批评性评论

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-20 DOI: 10.1016/j.dark.2025.102196

Salvatore Capozziello , Himanshu Chaudhary , Tiberiu Harko , G. Mustafa

We investigate whether the recent DESI DR2 measurements provide or not evidences for dynamical dark energy by exploring the ω₀ω_aCDM model and its extensions with free ∑m_ν and N_eff. Using a comprehensive MCMC analysis with a wide range of cosmological datasets including DESI DR2 BAO and Lyα data, CMB compressed likelihoods, BBN, cosmic chronometers, and multiple Type Ia supernova compilations we assess the statistical preference for departures from ΛCDM. We find that neither ΛCDM nor ω₀ω_aCDM reduces the sound horizon by the  ∼ 7 % required to alleviate the Hubble tension. DESI DR2 consistently favors the quadrant

ω_{0} > - 1

and ω_a < 0, indicating a preference for dynamical dark energy of the Quintom-B type at the  ≲ 3σ level for most dataset combinations, rising to  ∼ 3.8σ only when the DES-SN5Y supernova sample is included. Allowing ∑m_ν and N_eff to vary does not alter this preference and yields neutrino mass constraints consistent with ∑m_ν ≲ 0.1 eV, with nonzero masses detected up to the

\sim 1.5 σ +

level. The systematics diagnosis shows that the preference for dynamical dark energy is biased by the low-z (z < 0.1) DES-SN5Y SNe Ia sample from the CfA/CSP sample. When these low-z SNe Ia are excluded, our analysis no longer requires a dynamical dark energy and fully restores the ΛCDM model. The reconstructed evolution of ω(z) and f_DE(z) shows a transition from the phantom to the quintessence regime by crossing the phantom divide. Overall, DESI DR2 provides valuable new insights into dark energy but does not yet challenge the ΛCDM paradigm. Forthcoming Stage IV surveys including DESI DR3, Rubin Observatory, Euclid, Roman Space Telescope, and the Simons Observatory will be crucial for determining whether these hints of dynamical dark energy persist or are due to statistical fluctuations or residual systematics in low-redshift supernova samples.

我们通过探索ω0ωaCDM模型及其自由∑mν和Neff扩展来研究最近的DESI DR2测量是否为动态暗能量提供了证据。通过对一系列宇宙学数据集（包括DESI DR2 BAO和Lyα数据、CMB压缩可能性、BBN、宇宙天文钟和多个Ia型超新星汇编）的综合MCMC分析，我们评估了偏离ΛCDM的统计偏好。我们发现ΛCDM和ω0ωaCDM都没有将声视界降低 ~ 7%，以减轻哈勃张力。DESI DR2始终倾向于象限ω0>；−1和ωa <； 0，这表明在大多数数据集组合中，Quintom-B型的动态暗能量在 > 3σ水平上更受偏爱，只有在DES-SN5Y超新星样本中才上升到 ~ 3.8σ。允许∑mν和Neff变化不会改变这种偏好，并且产生与∑mν > 0.1 eV一致的中微子质量约束，在~ 1.5σ+水平上检测到非零质量。系统诊断表明，对动态暗能量的偏好受到来自CfA/CSP样品的低z (z <； 0.1)DES-SN5Y SNe Ia样品的偏差。当这些低z超新星Ia被排除在外时，我们的分析不再需要动态暗能量，并完全恢复ΛCDM模型。ω(z)和fDE(z)的重构演化表明，通过跨越幻相分界线，从幻相过渡到精粹态。总的来说，DESI DR2为暗能量提供了有价值的新见解，但还没有挑战ΛCDM范式。即将到来的第四阶段调查，包括DESI DR3，鲁宾天文台，欧几里得，罗马太空望远镜和西蒙斯天文台，对于确定这些动态暗能量的暗示是否持续存在，或者是由于统计波动或低红移超新星样本中的残余系统，将是至关重要的。

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引用次数: 0

Investigating the gross properties of gravastars in generalised cylindrically symmetric space-time within the framework of Rastall theory of gravity 在拉斯托引力理论的框架下研究广义圆柱对称时空中引力星的总体性质

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-19 DOI: 10.1016/j.dark.2025.102193

Debadri Bhattacharjee, Pradip Kumar Chattopadhyay

Present study explores the gravastars in the framework of modified theory of gravity, proposed by P. Rastall, in generalised cylindrically symmetric space-time. Following the Mazur-Mottola hypothesis, gravastars are classified as one of the most unique and exotic kind of compact objects, presenting themselves as a plausible alternative to black holes. In this study, we build upon the Mazur-Mottola framework of Gravitational Bose-Einstein Condensate (GBEC) stars by generalising it to a cylindrically symmetric spacetime within the framework of Rastall gravity to present a novel approach for estimating the mass limit of the thin shell of isotropic gravastars. We have ensured singularity-free solutions for the interior de-Sitter core, non-vanishing solutions for the thin shell and flat vacuum solution of the exterior region, within this parameter space. Under the framework of Rastall gravity and cylindrically symmetric spacetime, the Lanczos equations at the hypersurface junction

(r = R)

undergo significant modifications, leading to a revised form of the Darmois-Israel junction conditions. These modified junction conditions are utilised to investigate the influence of the Rastall parameter (ξ) on the mass of the thin shell and key characteristics of gravastars, including the shell’s proper length, energy, and entropy. Additionally, we propose a novel method for estimating the mass of the thin shell using the concept of surface redshift (Z_s). By adhering to the Buchdahl upper limit, Z_s < 2 for isotropic configuration, we have determined the mass bounds of the thin shell for various characteristic radii and values of the Rastall parameter (ξ).

本研究在广义圆柱对称时空中，在P. Rastall提出的修正引力理论的框架下，探讨了引力星。根据马祖尔-莫托拉假说，重力星被归类为最独特、最奇异的致密天体之一，似乎是黑洞的替代品。在本研究中，我们在引力玻色-爱因斯坦凝聚（GBEC）恒星的Mazur-Mottola框架的基础上，将其推广到拉斯托引力框架下的圆柱对称时空，提出了一种估计各向同性引力星薄壳质量极限的新方法。在这个参数空间内，我们保证了内部de-Sitter核心的无奇点解，薄壳的不消失解和外部区域的平面真空解。在Rastall重力和圆柱对称时空的框架下，对超表面结（r= r）处的Lanczos方程进行了重大修改，从而得到了修正形式的Darmois-Israel结条件。这些修正的结条件被用来研究拉斯托参数（ξ）对重力星薄壳质量和关键特性的影响，包括壳的固有长度、能量和熵。此外，我们提出了一种利用表面红移（Zs）的概念来估计薄壳质量的新方法。根据各向同性构型的Buchdahl上限Zs <； 2，我们确定了薄壳在各种特征半径和拉斯托参数（ξ）值下的质量边界。

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引用次数: 0

Gravitational lensing in a Kerr black hole within quantum Einstein gravity 量子爱因斯坦引力下克尔黑洞中的引力透镜

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-13 DOI: 10.1016/j.dark.2025.102191

Chen-Hao Xie, Yu Zhang, Bo-Li Liu, Peng-Fei Duan, Yu-Li Lou

The detailed study of the strong gravitational lensing of a Kerr black hole within quantum Einstein gravity (QEG) is performed. We calculate the photon sphere, the deflection angle of light, and observables on the equatorial plane under the strong deflection limit in a vacuum. The presence of quantum effects reduces the radius of the photon sphere, the light deflection angle, the ratio of magnification, the positions of relativistic images, and the time delays on the same side of the lens. However, it increases the separations, and the time delays on the opposite side of the lens. By modeling M87* and Sgr A* as the Kerr black hole within QEG, we find that the time delays are more significant in M87*, while other observables are more pronounced in Sgr A*. Furthermore, we consider the influence of plasma on the gravitational lensing effect. Plasma causes an additional deflection of light, increasing the ratio of magnification, image positions and the time delays, but decreasing the separations. More importantly, we calculate the time delays under the strong deflection limit in the presence of plasma and find that they increase with higher plasma concentrations. Finally, we calculate the weak deflection angle in the weak deflection limit. Our research may be helpful for evaluating the observational imprints of quantum effects on light propagation, as well as the influence of plasma around black holes on gravitational lensing.

对量子爱因斯坦引力（QEG）下克尔黑洞的强引力透镜进行了详细的研究。我们计算了真空中强偏转极限下的光子球、光的偏转角和赤道面上的观测值。量子效应的存在降低了光子球的半径、光的偏转角、放大倍率、相对论性像的位置以及透镜同侧的时间延迟。然而，它增加了分离，并在镜头的另一边的时间延迟。通过将M87*和Sgr A*作为QEG中的Kerr黑洞进行建模，我们发现M87*中的时间延迟更为显著，而Sgr A*中的其他观测值更为明显。此外，我们还考虑了等离子体对引力透镜效应的影响。等离子体引起额外的光偏转，增加了放大倍率、图像位置和时间延迟，但减少了分离。更重要的是，我们计算了等离子体存在时在强偏转极限下的时间延迟，发现它们随着等离子体浓度的增加而增加。最后，计算了弱挠度极限下的弱挠度角。我们的研究可能有助于评估量子效应对光传播的观测印记，以及黑洞周围等离子体对引力透镜的影响。

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引用次数: 0

Quasi-homologous evolution of dynamical relativistic stars in nonmetricity-induced gravity 非规度引力下动态相对论恒星的准同源演化

IF 6.4 2区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Physics of the Dark Universe

Pub Date : 2025-12-12 DOI: 10.1016/j.dark.2025.102190

S. Khan , Mohammad Alshammari , Othman Abdullah Almatroud , Z. Yousaf

The use of nonmetricity for modeling self-gravitational stellar fluids has become a compelling topic in relativistic astrophysics. In this respect, this study explores some viable non-static compact stellar configurations within the principles of linear and non-linear models of

f (Q)

theory. In particular, we formulate anisotropic, self-gravitational models (both dissipative and non-dissipative) using the well-motivated relativistic constraints known as the complexity-free configuration, along with the quasi-homologous condition. The resulting compact star models reveal important outcomes for the physical characteristics and evolution of dynamical, compact models exhibiting anisotropic stresses and non-uniform density distributions. Our work provides a fresh perspective on the development of highly dense matter objects under non-Riemannian geometrical influences by exploring the interaction between anisotropy, nonmetricity, quasi-homologous symmetry, and the complexity factor.

利用非规性来模拟自引力恒星流体已成为相对论天体物理学中一个引人注目的话题。在这方面，本研究在f(Q)理论的线性和非线性模型的原则下探索了一些可行的非静态致密恒星构型。特别是，我们利用被称为无复杂性配置的良好激发的相对论约束以及准同源条件，制定了各向异性的自引力模型（包括耗散和非耗散）。由此产生的致密恒星模型揭示了具有各向异性应力和非均匀密度分布的动态致密模型的物理特征和演化的重要结果。我们的工作通过探索各向异性、非度量性、准同源对称性和复杂性因素之间的相互作用，为非黎曼几何影响下高密度物质物体的发展提供了一个新的视角。

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引用次数: 0