arXiv 1503.089382015-03astro-ph.CO

热膨胀对小尺度密度扰动的影响

Effects of thermal inflation on small scale density perturbations

Sungwook E. Hong, Hyung-Joo Lee, Young Jae Lee, Ewan D. Stewart, Heeseung Zoe

发表信息：: JCAP 06 (2015) 002
DOI：: 10.1088/1475-7516/2015/06/002

摘要：

在热膨胀的宇宙学场景中，在原始膨胀和大爆炸核合成的辐射支配之间存在着模物质支配、热膨胀和平子物质支配的额外时代。在这些时期，小尺度上的宇宙学扰动可以进入和再退出视界，改变这些尺度上的功率谱。最大的修正标度$k_\mathrm{b}$与膨胀从收缩转变为膨胀时的视界尺寸相对应，此时膨胀从模量主导转变为热膨胀。我们解析地计算了从模控制到热膨胀的扰动演化，并计算了热膨胀结束时常辐射密度超曲面上的曲率扰动，以确定后期的曲率扰动。我们得到的传递函数抑制功率谱的一个因素$\sim 50$在$k \gg k_\mathrm{b}$，与$k_\mathrm{b}$对应的任何地方从兆秒差距到subparsec尺度取决于热膨胀的参数。因此，热膨胀可能会受到小尺度观测的限制或被检测到，如CMB畸变或21厘米氢线观测。

英文摘要：

In cosmological scenarios with thermal inflation, extra eras of moduli matter domination, thermal inflation and flaton matter domination exist between primordial inflation and the radiation domination of Big Bang nucleosynthesis. During these eras, cosmological perturbations on small scales can enter and re-exit the horizon, modifying the power spectrum on those scales. The largest modified scale, $k_\mathrm{b}$, touches the horizon size when the expansion changes from deflation to inflation at the transition from moduli domination to thermal inflation. We analytically calculate the evolution of perturbations from moduli domination through thermal inflation and evaluate the curvature perturbation on the constant radiation density hypersurface at the end of thermal inflation to determine the late time curvature perturbation. Our resulting transfer function suppresses the power spectrum by a factor $\sim 50$ at $k \gg k_\mathrm{b}$, with $k_\mathrm{b}$ corresponding to anywhere from megaparsec to subparsec scales depending on the parameters of thermal inflation. Thus, thermal inflation might be constrained or detected by small scale observations such as CMB distortions or 21cm hydrogen line observations.

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