发表机构
The University of Burdwan（巴尔达万大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究在Tsallis-Cirto熵启发修正引力中，通过修改Friedmann方程，发现该模型（$\beta\ne 1$）通过所有宇宙学测试，影响膨胀、结构增长和暗物质晕丰度，且大质量结构更少、形成更晚，符合层级形成模型。
AI 中文摘要
我们在Tsallis-Cirto修正引力框架内探索宇宙学动力学和结构形成，该框架带有一个受非广延统计启发的模型参数$\beta$。通过应用引力-热力学猜想，我们修改了Friedmann方程和Hubble参数的演化。通过使用平坦Friedmann-Lemaître-Robertson-Walker背景下的球对称坍缩方法制定扰动场方程，分析了Tsallis-Cirto熵对不同宇宙学参数的影响以及线性物质过密度的演化。我们提出了一种新颖且成熟的诊断方法，用于区分不同的宇宙学模型，并与平坦和非平坦$\Lambda$CDM情景进行比较，发现Tsallis-Cirto熵启发的修正宇宙学（$\beta\ne 1$）成功通过了所有测试，与平坦和非平坦$\Lambda$CDM模型相矛盾。该模型还满足宇宙在遥远未来达到热力学平衡的条件。此外，我们研究了该修正引力框架内的晕质量函数和星系团数量计数。所有发现都与基准$\Lambda$CDM轮廓进行了比较，表明添加的熵修正影响了膨胀历史、结构增长速率和暗物质晕丰度。我们发现，质量更大的结构丰度更低，并在更晚的时间形成，这与大尺度结构形成的层级模型一致。
英文摘要
We explore the cosmological dynamics and formation of structures within the Tsallis-Cirto modified gravity framework with a model parameter $β$ that is inspired by nonextensive statistics. By applying the gravity-thermodynamics conjecture, we modify the Friedmann equations and the evolution of the Hubble parameter. The impact of the Tsallis-Cirto entropy on different cosmographic parameters and the development of the linear matter overdensities have been analyzed by formulating perturbed field equations using the spherical collapse approach in a flat Friedmann-Lemaître-Robertson-Walker background. We present a novel and established diagnostic approach to distinguish among distinct cosmological models compared to flat and non-flat $Λ$CDM scenarios, discovering that the Tsallis-Cirto entropy-inspired modified cosmology ($β\ne 1$) successfully withstands all tests, contradicting both the flat and non-flat $Λ$CDM models. This model also meets the conditions for the Universe to reach thermodynamic equilibrium in the far future. Additionally, we investigate the halo mass function and cluster number counts within this modified gravity framework. All findings are compared to the fiducial $Λ$CDM profile, indicating that the added entropic correction affects the history of expansion, the growth rate of structures, and the dark matter halo abundance. We find that the more massive structures are less abundant and develop at later times, which aligns with the hierarchical model of formation of large-scale structures.
Comments21 pages, 21 figure
