A wide class of scalar field models including Quintessence and K-essence have the attractive property of tracker regimes, where the energy density stored in the field evolves so as to mimic that of the dominant background component. During this evolution, for a brief period of time, there is an increase in the energy density of the field as it spirals in towards its attractor solution. We show that when the peak of this energy density occurs around the epoch of equality, we can address a key requirement of early dark energy (EDE), postulated as a solution to the Hubble tension. In particular we demonstrate how this can occur in a wide class of Quintessence, axion and K-essence models, before showing that the Quintessence models suffer in that they generally lead to sound speeds incompatible with the requirements of EDE, whereas the K-essence and axion models can do a better job of fitting the data.

中文翻译：

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将解决方案扩展到哈勃张力的早期暗能量解决方案


包括 Quintessence 和 K-essence 在内的一类标量场模型具有跟踪器机制的吸引力，其中存储在场中的能量密度不断变化，以模仿主要背景成分的能量密度。在此演化过程中，在短时间内，场的能量密度会随着其螺旋向吸引子解而增加。我们证明，当这种能量密度的峰值出现在平等时代附近时，我们可以解决早期暗能量（EDE）的关键要求，假设作为哈勃张力的解决方案。我们特别演示了这种情况如何在各种 Quintessence、axion 和 K-essence 模型中发生，然后表明 Quintessence 模型的问题在于它们通常会导致声速与 EDE 的要求不兼容，而 K-essence 和轴子模型可以更好地拟合数据。