暴胀

在暴胀后数十万年，物质终于获得最后的胜利，并摆脱了辐射控制。

Several hundred thousand years after inflation , matter declared final victory and cut itself loose from radiation .

如果把标度因子a看作时间变量，则可得到成功的暴胀所需的标量场的初值。

If the scale factor a is thought of as a time variable , the initial values of ψ and x for the success of inflation are obtained .

由于对称性的自发破缺，在标量场的真空期待值近似为常数时，得到各向不同性的DeSitter解，这种真空暴胀将自行导致早期宇宙空间的各向同性化。

When the vacuum expectation value of the scalar field is approximately equal to a constant owing to the spontaneous symmetry breaking , we find a anisotropic de Sitter cosmological solution . The expansion isotropization is automatically obtained by this vacuum inflation .

暴胀宇宙中的体积粘滞流体

Bulk Viscous Fluid in an Inflating Universe

在标准理论中，加速膨胀发生在大霹雳之后，来源是一个理论学家特设的暴胀场。

In the standard theory , acceleration occurs after the big bang because of an ad hoc inflaton field .

根据为改进大爆炸理论而发展出来的暴胀理论，宇宙密度必定接近于临界密度，所以宇宙应是平坦的。

As an extension of the big bang theory , inflation theory predicts the universe density is rather close to the critical density . thus , the universe is flat .

通过引入暴胀假说，某些问题如视界疑难、平直性疑难以及磁单极子疑难等得到或部分得到解决。

By introducing the inflationary scenario , some of these problems for instance , horizon problem , flatness problem as well as magnetic monopole problem can be completely or partly resolved .

这个图像漂亮之处，在于它自动并入了标准暴胀理论的伟大洞见；也就是说，宇宙必须经历一段加速的时期，才能变得如此均匀且各向同性。

The beauty of this picture is that it automatically incorporates the great insight of standard inflationary theory-namely , that the universe had to undergo a period of acceleration to become so homogeneous and isotropic .

约在31×109a至30×109a前，地月距离突然暴胀了10多倍，导致太古代地壳构造活动和月海玄武岩喷发迅速终止；

Then the distance from Earth to Moon had suddenly inflated over 10 times between about 3 1 × 10 9 a and 3 0 × 10 9 a ago , which stopped the mobile period of Archean tectonics and the eruption of the Mare basalt in short order .