词条 超巨星
描述: 超巨星是体积最大、亮度最高的恒星。它们可能比太阳大几百倍，比太阳亮几千倍。它们占据赫兹普朗-拉塞尔图的顶部区域，绝对目视星等在-3 到-8 之间。超巨星的温度范围从大约3400开尔文（K）到超过20000开尔文（K）不等，它们要么是大质量恒星，要么处于恒星演化的后期阶段。超巨星可以根据它们的光谱来识别，超巨星可以通过它们的光谱来识别，其特征谱线对高亮度和低表面重力敏感：这些光谱线与较小恒星的线宽相比是较窄的。超巨星的典型例子包括猎户座的参宿四和造父变星。
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其他语言版本
- 阿拉伯语: نجم فائق الضخامة
- 德语: Überriesen
- 英语: Supergiant Star
- 波斯语: ستاره ابرغول
- 法语: Étoile supergéante
- 意大利语: Stella supergigante
- 日语: 超巨星 (外部链接)
- 韩语: 초거성
- 繁体中文: 超巨星
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The red supergiant Betelgeuse
图注： The image shows Betelgeuse, a red supergiant in the constellation Orion, observed by the Atacama Large Millimeter/submillimeter Array (ALMA). ALMA consists of many antennae spread across a plain in Northern Chile. The observations from all of these receivers is synthesised together by a central computer to form an image. The wide distances between the antennae mean that is can resolve very fine details.
Most stars we observe are just seen as points of light, but Betelgeuse is so large (with a radius about 1,400 times larger than the Sun) and is sufficiently nearby that it is one of the few stars to have been resolved to show it as an extended object.
Betelgeuse is a massive star, more than 14 times the mass of the Sun and is relatively young for a star (less than 14 million years old). However, its high mass led to it having a very hot core which burned through its hydrogen fuel quickly. It has since evolved through many stages and now appears as a red supergiant, it's final stage before exploding as a supernova. When such an explosion will happen is not known for certain, but it could be in around 100,000 years. Such an explosion would be visible from Earth, even during the day.
来源： ALMA (ESO/NAOJ/NRAO)/E. O’Gorman/P. Kervella
来源链接
相关图表
赫罗图
图注： 这张图展示了不同恒星温度和亮度。每个点的大小代表恒星的半径，颜色代表人眼所看到的颜色。恒星的颜色从淡蓝色到淡橙红色不等，没有恒星具有像红、绿或蓝这样的纯颜色，因为恒星的光谱包含了许多不同颜色的光。然而，最红的恒星通常被称为红恒星，最蓝的恒星被称为蓝恒星。为了展示不同类型的恒星，制作这个图表的恒星样本选择上并没有反映出每种类型恒星的实际数量比例。
从左上到右下是一条长长的恒星带，这些恒星在其核心燃烧氢气，这被称为主序。在这条线上，我们可以看到参宿三（Mintaka）、波江座α星（Achernar）、天狼星A（Sirius A）、太阳和比邻星（Proxima Centauri）等恒星。在主序线右下方的比邻星周围的天体被称为红矮星。在红矮星的右下方是Teide 1和Kelu-1 A。这两个天体是褐矮星，它们的质量太低，核心没有足够的热量来持续地进行氢融合。由于它们不燃烧氢，褐矮星不被认为是主序星。"褐矮星"这个名字与它们的颜色无关。
在主序星的上方，我们发现次巨星、巨星和超巨星。这些是已经完成了核心的氢燃烧并演化成更大天体的恒星。恒星的亮度取决于其温度和大小，因此巨星比具有较小半径但相同温度的恒星更亮。随着时间的推移，这些天体将走向生命的尽头，经历行星状星云阶段或变成超新星。以行星状星云阶段结束生命的恒星会形成一种叫做白矮星的恒星残骸。这种天体比相同温度的恒星小得多，因此更暗淡，并且位于主序星带的显著下方。以超新星结束生命的恒星会成为黑洞或中子星。这些在这个图表上没有显示。
来源： IAU OAE/Niall Deacon
