Warm inflation is a natural and well-motivated description of cosmic inflation which accounts for the inflaton dissipation and radiation production during the inflationary phase, neglected in the standard cold description. It results in crucial differences in the imprints on the Cosmic Microwave Background (CMB) radiation from the standard cold description. In this study, we consider warm inflation models with [Formula: see text] and [Formula: see text] potentials and estimate their model parameters consistent with CMB using the CosmoMC numerical code. These models are characterized by the inflaton self coupling, [Formula: see text], and the dissipation parameter, [Formula: see text], due to the inflaton’s dissipation into the other fields. Therefore, information about these physical parameters is essential from the perspective of the model building. In our analysis, we also calculate the spectral index, [Formula: see text], and the tensor-to-scalar ratio, [Formula: see text], for the mean values of the parameters and show that for the weak dissipative regime, [Formula: see text], is within the sensitivity of the next generation CMB polarization experiments, which is an important observational test for these models.

中文翻译：

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CMB热暴模型及其参数估计研究

暖暴胀是对宇宙暴胀的自然且有充分动机的描述，它解释了暴胀阶段的暴胀耗散和辐射产生，在标准冷描述中被忽略了。它导致宇宙微波背景 (CMB) 辐射上的印记与标准冷描述存在重大差异。在这项研究中，我们考虑具有 [公式：见文本] 和 [公式：见文本] 势的暖暴胀模型，并使用 CosmoMC 数字代码估计其模型参数与 CMB 一致。这些模型的特点是暴胀子自耦合[公式：见正文]和耗散参数[公式：见正文]，这是由于暴胀子在其他场中的耗散。所以，从模型构建的角度来看，有关这些物理参数的信息是必不可少的。在我们的分析中，我们还计算了参数平均值的光谱指数 [公式：参见文本] 和张量与标量比 [公式：参见文本]，并表明对于弱耗散状态， 【公式：见正文】，在下一代CMB极化实验的灵敏度范围内，是对这些模型的重要观测检验。