Description: 有質量的物體會使經過其引力影響範圍附近的光線發生彎曲。愛因斯坦的廣義相對論預言了這種效應，並在 1919 年日食期間首次被觀測到，測量發現太陽附近幾顆恆星發出的星光發生了彎曲。引力透鏡作用在質量非常大的物體上最為明顯，如星系或星系團。如果地球上的觀測者正在觀測一個光線被（"透鏡"）彎曲的遙遠天體，這個天體的成像會出現扭曲。這種扭曲總是意味著光線的（縮小）放大，通常能讓我們更好地看到暗淡的背景天體。當透鏡有足夠的質量集中在一個小角度區域時，同一背景物體就會產生多個圖像，每個圖像的光線到達觀察者的時間都不同。測量這些所謂的 "時間延遲 "是確定銀河系外哈勃常數值的最佳方法之一。另一方面，來自透鏡的多幅圖像可以讓我們利用建模分析精確地確定其質量。這是一種非常有用的方法，可以用來尋找星系的質量，特別是星系團的質量。

Related Terms:

• 暗物質
• 銀河系
• 星系團
• 超大質量黑洞
• 哈勃參數

Term and definition status: The original definition of this term in English have been approved by a research astronomer and a teacher
The translation of this term and its definition is still awaiting approval

This is an automated transliteration of the simplified Chinese translation of this term

The OAE Multilingual Glossary is a project of the IAU Office of Astronomy for Education (OAE) in collaboration with the IAU Office of Astronomy Outreach (OAO). The terms and definitions were chosen, written and reviewed by a collective effort from the OAE, the OAE Centers and Nodes, the OAE National Astronomy Education Coordinators (NAECs) and other volunteers. You can find a full list of credits here. All glossary terms and their definitions are released under a Creative Commons CC BY-4.0 license and should be credited to "IAU OAE".

If you notice a factual or translation error in this glossary term or definition then please get in touch.