Effects of thermal inflation on small scale density perturbations
Effects of thermal inflation on small scale density perturbations
复制标题
热膨胀对小尺度密度扰动的影响
DOI：
10.1088/1475-7516/2015/06/002
复制
发表时间：
2015
影响因子：
6.4
通讯作者：
Heeseung Zoe
中科院分区：
文献类型：
--
作者：
S. E. Hong;Hyun;Y. J. Lee;E. Stewart;Heeseung Zoe
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重新退出视界，修改这些尺度上的功率谱。最大的修正标度kb与膨胀从模主导向热膨胀转变时从紧缩向膨胀转变时的视界尺寸相接触。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0 - 5在k kb，与kb对应的任何地方从兆秒差距到subparsec尺度取决于参数的热膨胀。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。
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, kb, 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 0∼ 5 at k ≫ kb, with kb 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.
影响因子：
6.4
作者：
Prism Collaboration Philippe Andr'e;C. Baccigalupi;A. Banday;D. Barbosa;B. Barreiro;J. Bartlett;N. Bart
通讯作者：
Prism Collaboration Philippe Andr'e;C. Baccigalupi;A. Banday;D. Barbosa;B. Barreiro;J. Bartlett;N. Bart