Matter density perturbations in interacting quintessence models
Matter density perturbations in interacting quintessence models
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DOI：
10.1103/physrevd.74.043521
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发表时间：
2006-07
影响因子：
5
通讯作者：
G. Olivares;F. Atrio-Barandela;D. Pavón
中科院分区：
文献类型：
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作者：
G. Olivares;F. Atrio-Barandela;D. Pavón
人们提出了暗能量衰变为暗物质的模型来解决宇宙学中的巧合问题。我们研究了物质功率谱中这种耦合的影响。由于相互作用，与当今暗物质与暗能量比例相同的非相互作用模型相比，辐射主导状态下物质密度扰动的增长速度较慢。这种效应在小尺度上引入了与相互作用强度 c{sup 2} 成比例的功率谱阻尼，类似于超相对论中微子产生的效应。这种相互作用还将物质-辐射平等转移到更大的尺度。我们将相互作用的精华模型的物质功率谱与 2 度场星系红移巡天 (2dFGRS) 的测量结果进行了比较。数据对 c{sup 2}{<=}10{sup -3} 的值不敏感，但强烈约束较大的值。我们的研究专门针对在辐射统治期间具有恒定暗物质与暗能量比率的模型。
Models with dark energy decaying into dark matter have been proposed to solve the coincidence problem in cosmology. We study the effect of such coupling in the matter power spectrum. Because of the interaction, the growth of matter density perturbations during the radiation dominated regime is slower compared to noninteracting models with the same ratio of dark matter to dark energy today. This effect introduces a damping on the power spectrum at small scales proportional to the strength of the interaction, c{sup 2}, and similar to the effect generated by ultrarelativistic neutrinos. The interaction also shifts matter-radiation equality to larger scales. We compare the matter power spectrum of interacting quintessence models with the measurments of the 2-degree field galaxy redshift survey (2dFGRS). The data are insensitive to values of c{sup 2}{<=}10{sup -3} but strongly constrain larger values. We particularize our study to models that during radiation domination have a constant dark matter to dark energy ratio.