Dark energy model with very large-scale inhomogeneity
Dark energy model with very large-scale inhomogeneity
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DOI：
10.1103/physrevd.105.063518
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发表时间：
2021-11
影响因子：
5
通讯作者：
Yue Nan;Kazuhiro Yamamoto
中科院分区：
文献类型：
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作者：
Yue Nan;Kazuhiro Yamamoto
我们考虑了一个基于具有超大规模非均匀的超轻质量标量fi场的暗能量动力学模型。该模型可能会对宇宙微波背景强度和光度距离的各向异性产生明显的影响。我们将该模型描述为超视界尺度的宇宙学扰动，重点关注我们宇宙的局部区域。此外，我们还研究了非均匀暗能量后期演化的特征性质。我们的数值解表明，该模型可以模拟标准的Λ清洁发展机制宇宙学，同时包含空间相关的暗能量，并且模型参数在fl范围内是可容许的。通过对CMB各向异性的观测，我们在很大的尺度上限制了暗能量不均匀的幅度。我们还讨论了它们在光度距离估计中的fl关系。还表明(Cid：101)r对于背景展开并不重要，而Ωm确实在fl上显示了其在η0上的预期单位。为此，我们重点比较了编号为(1)、(3)、(4)、(6)和(11)的模型的条件，其中(ff：101)r的不同值很少改变η0；另一方面，编号(1)、(13)和(14)之间的比较显示，正如预期的那样，η0对Ωm略有依赖。尤其是，不。(11)是一个非常接近Λ清洁发展机制模型的模型，暗能量的状态方程与φ≈−1几乎不变，预示着未来的演化将迅速接近德西特展开。−5，(97)对于表IV中所有模型的红移z=3，讨论和结论我们建立了一个具有非均匀暗能量的宇宙学模型，该模型的暗能量来源于具有超大规模fi作用的动力学标量fl场，方法是将它们作为宇宙学微扰处理到均匀背景上，聚焦于局域可见宇宙。这个模型能够再现一个可观测的宇宙，它模拟了观测所青睐的宇宙中的Λ清洁发展机制fl，但在非常大的尺度上具有小幅度的不均匀性和各向异性。我们研究了支配宇宙演化的基本方程
We consider a dynamical model for dark energy based on an ultralight mass scalar field with very large-scale inhomogeneities. This model may cause observable impacts on the anisotropic properties of the cosmic microwave background (CMB) intensity and luminosity distance. We formulate the model as the cosmological perturbations of the superhorizon scales, focusing on the local region of our universe. Moreover, we investigated the characteristic properties of the late-time evolution of inhomogeneous dark energy. Our numerical solutions show that the model can mimic the standard ΛCDM cosmology while including spatially dependent dark energy with flexible ranges of the model parameters. We put a constraint on the amplitude of these inhomogeneities of the dark energy on very large scales with the observations of the CMB anisotropies. We also discuss their influence on the estimation of the luminosity distance. also indicate that (cid:101) r is not important for the background expansion, while Ω m does show its expected influence on η 0 . To see this, we focus on comparing the conditions of the models labeled with Nos. (1), (3), (4), (6), and (11), where different values of (cid:101) r rarely change η 0 ; on the other hand, a comparison among Nos. (1), (13), and (14) shows a slight dependence of η 0 on Ω m , as expected. Especially, No. (11) is a model extremely close to the ΛCDM model, and the EoS of dark energy is almost constant w φ ≈ − 1, predicting a future evolution quickly approaching the de Sitter expansion. − 5 , (97) at the redshift z = 3 for all models in Table I. V. DISCUSSIONS AND CONCLUSIONS We formulated a cosmological model with inhomogeneous dark energy sourced from a dynamical scalar field with extremely large-scale fluctuations, by handling them as cosmological perturbations to a homogeneous background to focus on a local observable universe. This model is capable of reproducing an observable universe that mimics the ΛCDM flat universe favored by the observations but with inhomogeneity and anisotropy of small amplitudes on very large scales. We investigated the basic equations governing the evolution of the universe for the