论文标题
Tachyon模型中的非线性球形崩溃，以及tachyon和深色能量模型中塌陷的比较
Non-linear spherical collapse in tachyon models, and a comparison of collapse in tachyon and quintessence models of dark energy
论文作者
论文摘要
我们研究暗物质和暗能量崩溃的扰动的演变。我们使用Rajvanshi和Bagla（2018）中概述的方法研究了暗能量的速元模型。我们与当前观察允许的模型合作。我们发现，与观察结果允许的典型模型一样，暗能量扰动不会以严重的方式影响暗物质中扰动的进化。对于此类模型，暗能量的扰动仍然很小。为了比较不同类别的暗能量模型，我们使用电势的重建并研究两个模型中相同扩展历史的暗物质和暗能量扰动。我们发现，暗物质扰动在相同的扩展历史记录中没有任何烙印的暗能模型的烙印：这很重要，因为我们可以使用任何方便的模型来研究暗物质的聚类。我们发现，暗能量扰动的演变带有一类模型的烙印，因为这些模型在Tachyon模型和典型模型中的生长不同。但是，在我们的宇宙中，使用（1+w）<< 1的这些减小之间的差异是使用扰动特征区分模型的前景。
We study evolution of perturbations in dark matter and dark energy for spherical collapse. We study Tachyon models of dark energy using the approach outlined in Rajvanshi and Bagla (2018). We work with models that are allowed by current observations. We find that as with Quintessence models allowed by observations, dark energy perturbations do not affect evolution of perturbations in dark matter in a significant manner. Perturbations in dark energy remain small for such models. In order to compare different classes of dark energy models, we use reconstruction of potentials and study dark matter and dark energy perturbations for same expansion history in the two models. We find that dark matter perturbations carry no imprint of the class of dark energy models for the same expansion history: this is significant in that we can work with any convenient model to study clustering of dark matter. We find that the evolution of dark energy perturbations carries an imprint of the class of models in that these grow differently in Tachyon models and Quintessence models. However, the difference between these diminishes for (1+w)<<1 and hence prospects for differentiating between models using characteristics of perturbations are limited in our Universe.
