Bulk viscous cosmological model in f(T,T) modified gravity

IF 4.2 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
Raja Solanki, Aaqid Bhat, P.K. Sahoo
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Abstract

This article explores the impact of bulk viscosity on understanding the universe’s accelerated expansion within the context of modified f(T,T) gravity, which is an extension of the f(T) gravitational theory, allowing a broad coupling between the energy–momentum scalar T and the torsion scalar T. We consider two f(T,T) functions, specifically f(T,T)=αT+βT and f(T,T)=αT+βT, where α and β are arbitrary constants, along with the fluid part incorporating the coefficient of bulk viscosity ζ=ζ0>0. We calculate the analytical solutions of the corresponding field equations for a flat FLRW environment, and then we constrain the free parameters of the obtained solution using CC, Pantheon+, and the CC+Pantheon+ samples. We perform the Bayesian statistical analysis to estimate the posterior probability utilizing the likelihood function and the MCMC random sampling technique. Further, to assess the effectiveness of our MCMC analysis, we estimate the corresponding AIC and BIC values, and we find that there is strong evidence supporting the assumed viscous modified gravity models for all three data sets. Also, we find that the linear model precisely mimics the ΛCDM model. We also investigate the evolutionary behavior of some prominent cosmological parameters. We observe that the effective equation of state parameter for both models predict the accelerating behavior of the cosmic expansion phase. In addition, from the statefinder test, we find that the parameters of the considered MOG models favor the quintessence-type behavior. Further, we observe that the behavior of Om(z) curves corresponding to both models represent a consistent negative slope across the entire domain. We infer that our cosmological setting utilizing f(T,T) gravity models with the viscous matter fluid embodies quintessence-like behavior and can successfully describe the late-time scenario.

f(T,T)中的块体粘性宇宙学模型
本文在修正的 f(T,T) 引力的背景下,探讨了体粘性对理解宇宙加速膨胀的影响。修正的 f(T,T) 引力是 f(T) 引力理论的扩展,允许能量-动量标量 T 和扭转标量 T 之间的广泛耦合。我们考虑了两个 f(T,T) 函数,即 f(T,T)=αT+βT 和 f(T,T)=α-T+βT,其中 α 和 β 是任意常数,流体部分包含体积粘度系数 ζ=ζ0>0。我们计算了平坦 FLRW 环境下相应场方程的解析解,然后使用 CC、Pantheon+ 和 CC+Pantheon+ 样本对所得解的自由参数进行约束。我们利用似然函数和 MCMC 随机抽样技术进行贝叶斯统计分析,以估计后验概率。此外,为了评估 MCMC 分析的有效性,我们估算了相应的 AIC 值和 BIC 值,结果发现有强有力的证据支持所有三个数据集的假定粘性修正重力模型。此外,我们还发现线性模型精确地模拟了ΛCDM 模型。我们还研究了一些重要宇宙学参数的演化行为。我们观察到,两个模型的有效状态方程参数都预测了宇宙膨胀阶段的加速行为。此外,通过状态探测器测试,我们发现所考虑的 MOG 模型的参数都偏向于 "精粹 "型行为。此外,我们还观察到,两种模型对应的 Om(z) 曲线在整个领域都呈现出一致的负斜率。我们推断,我们利用带有粘性物质流体的 f(T,T) 引力模型的宇宙学设置体现了类似五重子的行为,并能成功地描述晚时间情景。
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来源期刊
Astroparticle Physics
Astroparticle Physics 地学天文-天文与天体物理
CiteScore
8.00
自引率
2.90%
发文量
41
审稿时长
79 days
期刊介绍: Astroparticle Physics publishes experimental and theoretical research papers in the interacting fields of Cosmic Ray Physics, Astronomy and Astrophysics, Cosmology and Particle Physics focusing on new developments in the following areas: High-energy cosmic-ray physics and astrophysics; Particle cosmology; Particle astrophysics; Related astrophysics: supernova, AGN, cosmic abundances, dark matter etc.; Gravitational waves; High-energy, VHE and UHE gamma-ray astronomy; High- and low-energy neutrino astronomy; Instrumentation and detector developments related to the above-mentioned fields.
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