The impact of anisotropy on the Ricci dark energy cosmologies is investigated where it is assumed that the geometry of the universe is described by Bianchi type I (BI) metric. The main goal is to determine the astrophysical constraints on the model by using the current available data as type Ia supernovae (SNIa), the Baryon Acoustic Oscillation (BAO), and the Hubble parameter H(z) data. In this regard, a maximum likelihood method is applied to constrain the cosmological parameters. Combining the data, it is found out that the allowed range for the density parameter of the model stands in − 3.6 × 10−3 ≲ Ω σ0 ≲−2.6 × 10−3. With the help of the Supernova Legacy Survey (SNLS) sample, we estimate the possible dipole anisotropy of the Ricci dark energy model. Then, by using a standard χ2 minimization method, it is realized that the transition epoch from early decelerated to current accelerated expansion occurs faster in Ricci dark energy model than ΛCDM model. The results indicate that the BI model for the Ricci dark energy is consistent with the observational data.

中文翻译：

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Bianchi I 型模型中 Ricci 暗能量宇宙学的约束

研究了各向异性对 Ricci 暗能量宇宙学的影响，假设宇宙的几何形状由 Bianchi I 型 (BI) 度量来描述。主要目标是通过使用当前可用的数据作为 Ia 型超新星 (SNIa)、重子声学振荡 (BAO) 和哈勃参数来确定模型的天体物理约束H(z)数据。在这方面，应用最大似然法来约束宇宙学参数。结合数据发现模型的密度参数允许范围为 - 3.6 × 10-3 ≲ Ω σ0 ≲-2.6 × 10-3. 在超新星遗产调查 (SNLS) 样本的帮助下，我们估计了 Ricci 暗能量模型可能的偶极各向异性。然后，通过使用标准χ2最小化方法，实现了从早期减速到当前加速膨胀的过渡时期在 Ricci 暗能量模型中发生得比Λ清洁发展机制模型。结果表明，Ricci暗能量的BI模型与观测数据一致。