In this study, we provide an alternatively reformulated interpretation of Gibbons–Hawking radiation as well as inflation. By using a spacetime quantization procedure, proposed recently by L.C. Céleri et al., in anti-de Sitter space we show that Gibbons–Hawking radiation is an intrinsic property of the concerned space, that arises due to the existence of a scalar field whose quanta “carry” a length $l$ (i.e. the radius of the hyperboloid curvature). Furthermore, within the context of Tsallis q-framework, we propose an inflationary model that depends on the non-extensive parameter $q$. The main source of such an inflation is the same scalar field mentioned before. Being constrained by the observational data, the q-parameter along with the rest of the model’s parameters has been used to estimate the time at which inflation ends as well as the reheating temperature. The latter is found to be related to Gibbons–Hawking temperature. Thus, the present model offers an alternative perspective regarding the nature of the cosmic background radiation (CMB).

在这项研究中，我们对吉本斯-霍金辐射以及通货膨胀提供了一种替代性的重新解释。通过使用LCCéleri等人最近在反de Sitter空间中提出的时空量化程序，我们证明了Gibbons-Hawking辐射是有关空间的固有特性，这是由于存在一个标量场而导致的。 “携带”一段$升$（即双曲面曲率半径）。此外，在Tsallis q框架的背景下，我们提出了一个依赖于非扩展参数的通胀模型$q$。这种通货膨胀的主要来源是前面提到的相同的标量场。受观测数据的约束，q参数以及模型的其余参数已被用于估计充气结束的时间以及再加热温度。发现后者与吉本斯-霍金温度有关。因此，本模型提供了关于宇宙背景辐射（CMB）性质的另一种观点。