數學與物理學中，一個n維德西特空間（，標作dSn）為一最大對稱的勞侖茲流形，具有正常數的純量曲率。

主要應用是在廣義相對論作為最簡單的宇宙數學模型。

「德西特」是以威廉·德西特（1872–1934）為名，他與阿爾伯特·愛因斯坦於1920年代一同研究宇宙中的時空結構。

以廣義相對論的語言來說，德西特空間為愛因斯坦場方程式的最大對稱真空解：具正宇宙學常數對應正真空能量密度和負壓。

In , n-dimensional de Sitter space (often abbreviated to dSn) is a maximally symmetric  with constant positive . It is the Lorentzian analogue of an  (with its canonical ).

The main application of de Sitter space is its use in ,  where it serves as one of the simplest mathematical models of the universe consistent with the observed . More specifically, de Sitter space is the maximally symmetric  of  with a positive   (corresponding to a positive vacuum energy density and negative pressure). There is cosmological evidence that the universe itself is , i.e. it will evolve like the de Sitter universe in the far future when  dominates.

de Sitter space and  are named after  (1872–1934), professor of astronomy at Leiden University and director of the 莱顿天文台. Willem de Sitter and Albert Einstein worked closely together in Leiden in the 1920s on the spacetime structure of our universe. de Sitter space was also discovered, independently, and about the same time, by 图利奥·列维-齐维塔.

定義 
de Sitter space can be defined as a  of a generalized 閔考斯基時空 of one higher . Take Minkowski space R1,n with the standard :

de Sitter space is the submanifold described by the  of one sheet

where  is some nonzero constant with its dimension being that of length. The  on de Sitter space is the metric induced from the ambient Minkowski metric. The induced metric is  and has Lorentzian signature. (Note that if one replaces  with  in the above definition, one obtains a  of two sheets. The induced metric in this case is , and each sheet is a copy of . For a detailed proof, see .)

de Sitter space can also be defined as the   of two s, which shows that it is a non-Riemannian .

, de Sitter space is  (so that if  then de Sitter space is ).

Properties
The  of de Sitter space is the 勞侖茲群 . The metric therefore then has  independent 基灵矢量场s and is maximally symmetric. Every maximally symmetric space has constant curvature. The 黎曼曲率張量 of de Sitter is given by

(using the sign convention  for the Riemann curvature tensor). de Sitter space is an  since the  is proportional to the metric:

This means de Sitter space is a vacuum solution of Einstein's equation with cosmological constant given by

The  of de Sitter space is given by

For the case , we have  and .

Coordinates

Static coordinates 
We can introduce   for de Sitter as follows:

where  gives the standard embedding the -sphere in Rn−1. In these coordinates the de Sitter metric takes the form:

Note that there is a  at .

Flat slicing 
Let

where .  Then in the  coordinates metric reads:

where  is the flat metric on 's.

Setting , we obtain the conformally flat metric:

Open slicing 
Let

where  forming a  with the standard metric .  Then the metric of the de Sitter space reads

where

is the standard hyperbolic metric.

Closed slicing 
Let

where s describe a .  Then the metric reads:

Changing the time variable to the conformal time via  we obtain a metric conformally equivalent to Einstein static universe:

These coordinates, also known as "global coordinates" cover the maximal extension of de Sitter space, and can therefore be used to find its 彭罗斯图.

dS slicing 
Let

where s describe a .  Then the metric reads:

where

is the metric of an  dimensional de Sitter space with radius of curvature  in open slicing coordinates.  The hyperbolic metric is given by:

This is the analytic continuation of the open slicing coordinates under  and also switching  and  because they change their timelike/spacelike nature.

See also
 反德西特空間
 
 AdS/CFT对偶

參考資料

延伸閱讀

外部鏈接 
  Simplified Guide to de Sitter and anti-de Sitter Spaces  A pedagogic introduction to de Sitter and anti-de Sitter spaces. The main article is simplified, with almost no math. The appendix is technical and intended for readers with physics or math backgrounds.

Exact solutions in general relativity
Differential geometry
Minkowski spacetime