This study belongs to a series devoted to using Szekeres inhomogeneous models to develop a theoretical framework where observations can be investigated with a wider range of possible interpretations. We look here into the growth of large-scale structure in the models. The Szekeres models are exact solutions to Einstein's equations that were originally derived with no symmetries. We use a formulation of the models that is due to Goode and Wainwright, who considered the models as exact perturbations of an FLRW background. Using the Raychaudhuri equation, we write for the two classes of the models, exact growth equations in terms of the under/overdensity and measurable cosmological parameters. The new equations in the overdensity split into two informative parts. The first part, while exact, is identical to the growth equation in the usual linearly perturbed FLRW models, while the second part constitutes exact non-linear perturbations. We integrate numerically the full exact growth rate equations for the flat and curved cases. We find that for the matter-dominated era, the Szekeres growth rate is up to a factor of three to five stronger than the usual linearly perturbed FLRW cases, reflecting the effect of exact Szekeres non-linear perturbations. The growth is also stronger than that of the non-linear spherical collapse model, and the difference between the two increases with time. This highlights the distinction when we use general inhomogeneous models where shear and a tidal gravitational field are present and contribute to the gravitational clustering. Additionally, it is worth observing that the enhancement of the growth found in the Szekeres models during the matter-dominated era could suggest a substitute to the argument that dark matter is needed when using FLRW models to explain the enhanced growth and resulting large-scale structures that we observe today (abridged)
A ready-to-fit inhomogeneous cosmological model: The axially symmetric Szekeres spacetime
Laboratoire d’étude de l’Univers et des phénomènes eXtrèmes (LUX), Observatoire de Paris-PSL, UMR 8262 CNRS, Sorbonne Université（宇宙与极端现象研究实验室（LUX），巴黎天文台-PSL，CNRS联合研究单位8262，索邦大学）
An effective $\boldsymbolΛ$-Szekeres modelling of the local Universe with Cosmicflows-4
University of Canterbury（坎特伯雷大学）；The University of Queensland（昆士兰大学）；Aix Marseille Universite, CNRS/IN2P3, CPPM（艾克斯-马赛大学，法国国家科学研究中心/欧洲核子研究组织，粒子物理中心）；Leibniz Institut fur Astrophysik Potsdam (AIP)（波茨坦阿基米德天体物理研究所）
本文利用Cosmicflows-4的数据，通过多结构Λ-塞克雷斯块的叠加模型，研究局部宇宙结构对宇宙学观测的影响，发现考虑局部结构会增加哈勃张力，使哈勃常数的最佳拟合值变化约0.5 km s⁻¹ Mpc⁻¹。
Supermassive black hole seeds from direct collapse of CDM-curvature peaks
University of Canterbury（坎特伯雷大学）；Institute of Cosmology & Gravitation, University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）；INFN Sezione di Trieste（的里雅斯特意大利国家核物理研究所）；Rikkyo University（立教大学）；iCLA, Yamanashi Gakuin University（山梨学院大学国际基督教学习中心）；Centre for Theoretical Physics, Jamia Millia Islamia（贾米亚米利亚伊斯兰大学理论物理中心）
Sensitivity toward dark matter annihilation imprints on 21-cm signal with SKA-Low: A convolutional neural network approach
Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences (HIAS-UCAS)（中国科学院大学杭州高等研究院）；University of Chinese Academy of Sciences（中国科学院大学）；International Centre for Theoretical Physics Asia-Pacific (ICTP-AP)（亚太理论物理中心）；Gifu Shotoku Gakuen University（岐阜女子大学）；Institute for Advanced Research, and Kobayashi Maskawa Institute, Nagoya University（名古屋大学先进研究院及小林–益川研究所）
