AI 中文总结
本文将单模框架引入带CW势的BD理论，求解平坦FRW时空场方程，所得参数理论预测与Planck2018、DESI2024、ACT2025观测数据最佳拟合，解决宇宙学常数精细调节问题。
AI 中文摘要
作为广义相对论的替代引力理论，布兰斯-迪克（Brans-Dicke, BD）标量-张量模型广为人知，其中BD参数控制最佳拟合观测数据，其宇宙学模型在文献中已被广泛研究。另一方面，科尔曼-温伯格（Coleman-Weinberg, CW）自相互作用标量场势源自费曼图的辐射修正，用于描述最佳拟合的宇宙暴胀阶段与再加热阶段。该势具有相对于希格斯势的对数项，即使对于无质量玻色子也适用，从粒子物理角度看，它通常用于描述希格斯机制与有质量戈德斯通玻色子的产生。作为描述宇宙暴胀的基础模型，宇宙学常数被用于描述德西特空间，其中宇宙学常数扮演暗能量密度的角色。由于宇宙学常数存在层级问题，且被加入爱因斯坦方程却未说明其起源，阿尔伯特·爱因斯坦本人首次提出了单模框架，据此宇宙学常数由一个积分常数产生，该思路可解决宇宙学常数参数的“精细调节”问题。因此，我们将该思路应用于存在CW势的BD理论中，考虑宇宙暴胀的慢滚参数，获得了平坦罗伯逊-沃克时空的场方程的合适解，进而得到该解参数的理论预测与Planck2018、DESI2024及ACT2025观测数据的最佳拟合对应关系。
英文摘要
As alternative gravity theories with respect to the general relativity, the Brans-Dicke (BD) scalar tensor model is well known for which the BD parameter is controller the best fit observational data and so its cosmological model is studied in the literature well. On the other side, the Coleman Weinberg (CW) self-interaction scalar field potential coming from radiation corrections of Feynman diagrams is used to describe the best fit cosmic inflation phase and reheating phase. This has a logarithmic term with respect to the Higgs potential and it is applicable even for massless bosons. From particle physics point of view, this is used usually to describe the Higgs mechanism and creation of massive Goldstone bosons. As a basic model to describe the cosmic inflation the cosmological constant is used to describe the de Sitter space where the cosmological constant play as dark energy density. Since, the cosmological constant is a hierarchy problem and it is added in the Einstein equation without to describe that where that is come originally? at a first time the Albert Einstein himself proposed a uni-modular frame for which the cosmological constant generate from a integral constant. This idea is very well because it resolve `fine tuning` problem of the cosmological constant parameter. Hence we use this idea for the BD theory in presence of the CW potential and obtained suitable solutions of the field equations for a flat Robertson-Walker space time by regarding the slow roll parameters of cosmic inflation and then we find the best fit correspondence between the theoretical predictions of the parameters of the solutions and the Planck2018, DESI2024, and ACT2025 observational data.
Comments19 pages, 6 figures, 1 table
