暗能量的晚期涌现及其与暗物质的相互作用
Late-Time Emergence of Dark Energy and Its Interaction with Dark Matter
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- Liaoning Normal University（辽宁师范大学）
- Presidency University（总统大学）
- Durban University of Technology（德班理工大学）
- Instituto de Física Corpuscular (CSIC-Universitat de València)（粒子物理研究所（瓦伦西亚大学-西班牙高等科学研究委员会））
- University of Sheffield（谢菲尔德大学）
- Brainware University（Brainware大学）
机构由 AI 辅助整理，请以论文原文为准。
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中文总结 AI 辅助
该研究提出暗能量晚期涌现且与暗物质相互作用的模型，结合多组宇宙学数据约束后发现相互作用参数偏离零但模型未优于ΛCDM等标准模型，凸显其解决宇宙学张力的局限性。
中文摘要 AI 辅助
我们提出了暗能量（DE）与暗物质（DM）之间的一种相互作用场景，其中暗能量具有涌现性质，即暗能量在早期宇宙中不存在，仅在晚期才发挥作用。我们考虑两种特定的涌现暗能量模型：一种无自由参数，另一种包含两个描述转变速度和转变时期的参数。我们使用Planck 2018发布的宇宙微波背景（CMB）测量数据、DESI DR2的重子声学振荡数据，以及三组不同的Ia型超新星汇编（PantheonPlus、DES-Dovekie和Union3）来约束这两种场景。我们的分析表明，当前的宇宙学探针无法紧密约束转变速度。对于两种场景，当CMB数据与这些额外探针中的任意一种结合时，相互作用参数的后验分布在95%置信水平以上偏离零，偏好的方向对应能量从暗能量转移到暗物质。仅CMB数据会产生较高的H₀值，与局地测量结果一致；当加入DESI数据时，这种效应会减弱；一旦加入超新星数据，该效应便会消失。相反，在组合数据集中，成团参数S₈始终向较低值偏移，且与负相互作用的偏好相关。然而，根据Δχ²_min和贝叶斯证据，没有一种相互作用模型比ΛCDM或w₀w_aCDM更受青睐，这表明这种相互作用并不能拯救这些涌现暗能量模型。因此，我们的结果凸显了这些场景在解决当前宇宙学张力方面的局限性，同时指出未来数据在进一步评估其可行性方面的关键作用。
英文摘要
We present an interacting scenario between dark energy (DE) and dark matter (DM), where DE has an emergent nature, that means, DE was absent in the early universe but it becomes effective only at late times. We consider two specific emergent DE models, one with no free parameters and the other featuring two parameters describing the speed and epoch of the transition. We constrain both scenarios using the cosmic microwave background (CMB) measurements from the Planck 2018 release, baryon acoustic oscillations from DESI DR2, and three different compilations of Type Ia supernovae (PantheonPlus, DES-Dovekie, and Union3). Our analysis indicates that current cosmological probes are not able to tightly constrain the speed of the transition. For both scenarios, the posterior distribution of the interaction parameter is shifted away from zero at more than 95\% CL whenever the CMB data are combined with any of these additional probes, with the preferred direction corresponding to a transfer of energy from DE to DM. While CMB alone yields a high value of $H_0$, in agreement with local determinations, this effect is reduced when DESI is added and disappears once supernova data are included. In contrast, the clustering parameter $S_8$ is consistently shifted toward lower values in the combined datasets, and it is correlated with the preference for a negative interaction. However, according to the $Δχ^2_{\rm min}$ and Bayesian evidence, none of the interacting models is favored over $Λ$CDM or $w_0w_a$CDM, indicating that the interaction does not rescue these emergent DE models. Our results therefore highlight the limitations of these scenarios in addressing current cosmological tensions, while pointing to the crucial role of future data in further assessing their viability.
