1) inflation
[英][ɪn'fleɪʃn] [美][ɪn'fleʃən]
暴涨
1.
when scalar field as outer field is inhomogeneous and is regarded as torsion potential of space-time s torsion, the exponential multiplying power-law inflation may occur in the very early stage of the universe.
证明了在非均匀球对称的Tolman-Bondi时空中,应用Brans-Dicke理论,当作为外场的B-D标量场是非均匀的,且将其视为时空挠率的挠率势时,选取合适的拉氏作用量,则极早期宇宙将以指数幂律倍增的形式发生暴涨。
2.
When matter spin interaction is considered,the energy content of the universe is spin dominated,effective inflation can occur and the universe is radiation and dust dominated at a sufficiently early epoch.
Gasperini给出的自洽的引力场方程,当考虑自旋与自旋的相互作用时,发现自旋密度对极早期宇宙起支配作用,是引起暴涨的根本原因,而且极早期宇宙是以辐射和尘埃为主,同时,由该模型得到一个非零的最小“宇宙半径”和初始密度。
4) chaotic inflation model
暴涨模型
1.
Adopting the Friedmann-Robertson-Walker model,we present a new exact solution to Einstein s equation that describes the evolution of the cosmological chaotic inflation model,and calculate the spectral indices ns of the scalar density fluctuation and the gravitational wave spectral index ng.
采用Friedmann-Robertson-Walker模型,提出了一个新的描述宇宙浑沌暴涨模型演化的Einstein场方程解,并计算了标量密度涨落的光谱指数ns和引力波光谱指数ng,得到ns的值很好地符合宇宙背景观测卫星观测到的值。
5) number of inflationary efolds
暴涨指数
1.
Particularly,the expected number of inflationary efolds is studied carefully.
回顾了现代宇宙学的历史和现状,从Friedmann方程出发,将标量场的量子涨落作为Gaussian白噪声,建立了反映宇宙暴涨过程的Langevin方程,得到尺度因子的均值、自相关系数和方差;特别是详细计算了暴涨指数,发现用这种方法得到的暴涨指数与经典结果差异甚微。
6) inflationary universe
暴涨宇宙
补充资料：暴涨
①（水位）急剧上升：河水～。②（物价等）突然大幅度地上升：米价～。
说明：补充资料仅用于学习参考，请勿用于其它任何用途。
参考词条