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tokenpocket苹果怎么下载|rigel

作者： tokenpocket苹果怎么下载

2024-03-07 20:52:17

参宿七（蓝超巨星）_百度百科

蓝超巨星）_百度百科网页新闻贴吧知道网盘图片视频地图文库资讯采购百科百度首页登录注册进入词条全站搜索帮助首页秒懂百科特色百科知识专题加入百科百科团队权威合作下载百科APP个人中心参宿七是一个多义词，请在下列义项上选择浏览（共2个义项）展开添加义项参宿七播报讨论上传视频蓝超巨星收藏查看我的收藏0有用+10本词条由“科普中国”科学百科词条编写与应用工作项目审核。参宿七，即猎户座β（Beta Orionis），其天文学特有名称是Rigel，源自阿拉伯语，有“左腿”的意思。全天最亮的二十颗恒星中排行第七名，又是最亮的蓝超巨星，虽然名为β星，但绝大多数时候比α星参宿四还要亮（因为参宿四是一颗不规则变星，参宿七的亮度也会变化）。参宿七的视星等约为0.13，绝对星等为-7.92 [9]，距离地球约863光年。其光谱类型属于B8Ia [7]，论恒星阶段，参宿七属于超巨星。论恒星大小，参宿七属于蓝超巨星，光度为太阳的12万倍 [9]，它是猎户座最亮星。中文名参宿七外文名Rigel别名猎户座β（β Orionis）、猎户座19 [8]（19 Orionis）分类恒星质量约 21 M⊙ [7]（±3）直径1.07184✕108 km表面温度约 12100 K [7]（±150）视星等约 0.13 等 [9]（0.05 - 0.18）绝对星等-7.92 等 [9]（± 0.28）赤经5时14分32.30秒赤纬-8°12′06″距地距离860 光年 [9]（± 80）目录1恒星简介2观测资料▪参宿七A▪参宿七B▪参宿七C3性质▪太空光度学▪光谱学4系统5观测▪可见性▪简述▪观测方位6语源学和文化意义▪英文语源▪欧洲文化▪东方和南亚恒星简介播报编辑参宿七（英语：Rigel A），在拜耳命名法中称为猎户座β（β Ori, β Orionis），是猎户座中最亮的恒星，并且是全天第7亮星，它的视星等约为0.13等。从地球上观察，这是个三合星的系统，主星为参宿七A（Rigel A），是颗绝对星等-7.92等的超巨星 [9]，亮度为太阳的130,000倍 [1]，是颗有固定周期的天鹅座α型变星。以小型望远镜就可以看见的参宿七B，本身就是光谱联星，由两颗光谱类型为B9的蓝白色恒星组成。虽然在拜耳命名法为β星，但它始终比猎户座α（参宿四）明亮。从1943年以来，它的光谱就被当成其它恒星光谱分类的校准光谱之一。参宿七是著名的蓝白色超巨星，位于猎户座的右下角，目视星等约在0.05～0.18之间变化，绝对星等-7.92 [9]。表面温度1.13万摄氏度，半径为太阳的77倍，总光度为太阳的12万倍，距离地球863光年。观测表明，参宿七不仅连续地吹出很强的星风，还以间断的方式抛出物质，形成一个膨胀的气壳。它最亮时成为猎户座的第一亮星，光度变化规律有待研究 [2]。参宿七观测资料播报编辑参宿七A历元：J2000星座：猎户座赤经： 05h 14m 32.30s赤纬：−08° 12' 06"视星等：(V) 0.12/8.44光谱分类： B8IabB-V色指数：−0.03U-B 色指数：−0.66变星类型：Slightly irregular径向速度：(Rv) 20.7 km/s自行：(μ) RA: 1.87 mas/yrDec.：−0.56 mas/yr视差：(π) 4.22 ± 0.81 mas距离：860 ± 80 ly (260 ± 20 pc) [9]绝对星等(MV)：−7.92 ± 0.28 [9]质量：21 ±3 M☉ [7]半径：78.9 ± 7.4 R☉ [7]光度：126,000(bolometric) L☉寿命：小于1000万年温度：12100 ± 150 K其他命名：猎户座右下角最亮星即参宿七β Orionis, 19 Ori, Algebar, Elgebar, HD 34085, HR 1713, HIP 24436, SAO 131907参宿七B参宿七B 的星等为6.7，如果不是离参宿七A 那么近的话，就很容易被小型望远镜看到。参宿七B 比它的邻居弱440倍，因此很难用小于6英寸的望远镜看到它。它的自行运动与参宿七A 相似，两颗恒星的轨道周期至少为18000年。参宿七B 是双线光谱双星，这意味着两颗恒星的光谱线都是可见的。两颗恒星都很热，光谱分类为 B9，它们被认为与参宿七形成了一个三星系统。 [7]参宿七C参宿七C和参宿七B之间的距离不到0.1到0.3弧秒。2009年的观察显示，参宿七B 和参宿七C 具有几乎相同的性质，而且只相隔0.124弧秒。这两颗恒星相互环绕的周期为63年。 [7]性质播报编辑以光谱估计参宿七的距离在700和900光年（210和280秒差距）之间，而依巴谷卫星的视差测量给出的距离是860光年（260秒差距），误差范围约为9%。它是一颗蓝超巨星，质量大约是18太阳质量，闪耀着大约117,000倍太阳的光度。干涉仪测量出它的角直径，在修正周边昏暗效应之后，大约是2.75 ± 0.01mas。在前述估计的距离下，它的半径相当于74个太阳半径。如果在1天文单位的距离上，它的角直径是35°，并且视星等是 -38等。因为它是在星云状物质中穿越的明亮天体，参宿七照亮在他附近的一些尘云，最明显的是IC 2118（女巫头星云）。参宿七也与猎户座大星云相关联－－或多或少有相同的视线速度－－几乎是两倍远的距离。尽管距离不同，参宿七通过空间的距离投影和对它年龄的估计，认为它是来自星云。由于这个结果，参宿七有时被分类为脱离猎户座OB1星协成员，还有天空中许多明亮的恒星；更具体的说，它是金牛-猎户R1星协的成员，是最近新设立（形成）的OB星协，包含了更多接近星云的亮星。参宿七是一颗超巨星变星，它的变化肇因于与天津四，脉动变星天鹅座α型变星的原型，相似的恒星脉动。参宿七的径向速度变化证明它至少有19种非径向模式的同时摆动，变异的时间范围从1.2天至74天。它是颗值得注意的蓝超巨星，因为它产生脉动的能量感觉上是来自核心燃烧中的氢壳层。已知参宿七的系统有三颗恒星，也有人认为系统中可能还有第四颗，但普遍认为这是主星的变异，引发表面的物理脉动造成的一种曲解 [3]。太空光度学参宿七2009年，加拿大的MOST卫星对参宿七观测达28天之久。这颗蓝超巨星的光度变化仅有千分之一星等的水平，逐渐改变光通量是这种长周期脉动变星的一种显著模式。光谱学参宿七被逐出的气体壳层包围着。出现这种情况是因为当一颗红巨星成为蓝巨星时，因此之前由红巨星缓慢吹出的气体会被蓝巨星高速吹出的气体挤压。参宿七的光谱是被确认是B8Ia [7]，并且通常被当成确认超巨星光谱类型的标准定义点。然而，因为大气层周期性的喷发，光谱的细节经常有很大的变化。谱线显示的发射、吸收、谱线致宽、天鹅P和逆天鹅P轮廓都没有可观察到的周期性。这样的结果导致在分类时的B8Iab、B8Iae会因人而异，或是混淆不清。系统播报编辑至少从1831年起就已经知道参宿七是目视联星，F. G. W.斯特鲁维对这个系统进行了测量。尽管参宿七B并不是很暗，6.7等，但靠在亮度是它500倍的参宿七A旁边，使它成为150 mm（5.9英寸）小望远镜挑战的目标 150 mm（5.9英寸）。不过一架品质良的 7 cm（2.8英寸）望远镜，使用150×，在良好的视宁度下，还是可以看见参宿七B。以参宿七的距离估计参宿七B与主星相距大约2,200天文单位（光程12.7天）；由于它们共享自行，因此观察不到它的轨道运动也不足为奇。参宿七B本身也是光谱联星，组成的两颗主序星以9.8天的轨道周期绕着它们质量中心运转。这两颗星的光谱类型都是B9V，质量分别是太阳的2.5和1.9倍。从19世纪晚期到20世纪初，长期以来都在争议参宿七B可能是可见的双星。一些有经验的观测者声称它们确实看见了两颗恒星，但大多数的观测者都无法确认；事实上，认为是联星的拥护者也无法重复他们结果。现已排除参宿七B有目视可见伴星的可能性。观测播报编辑可见性在天文学的数据库SIMBAD中，参宿七的视星等是0.12，使他成为在天球上除了太阳之外平均第六亮的天体－只比织女星和小犬头部的南河三暗（比御夫座的双星五车二的个别恒星明亮，但低于它们的合成星等）。它是颗光度在0.05-0.18等之间变化的不规则脉动变星 [4]。参宿四每年在12月12日的子夜和1月24日21:00过中天，所以在北半球的冬天或南半球的夏天是最适宜观赏它的时段 [5]。在南半球，参宿七是猎户座升起来之后，在这个星座内能看见的最亮一颗恒星 [6]。简述猎户座猎户座，是夜空中是容易辨认的星座之一。不过猎户座奥瑞恩的恒星和星云看上去不如在相片上那么鲜艳，庞大的低温红色参宿四泛着淡红色，是左边最明亮的星星。奥瑞恩更多的是蓝色的高温恒星，比参宿四更亮的是右下方的参宿七，参宿五位于右上方，参宿六位于左下方。构成猎户座的腰带（从下往上）分别是参宿一，参宿二和参宿三。这三颗恒星距离我们均是大约一千五百光年，它们诞生在这个星座的星际云。猎户两腿中间那颗像星星的东西，如果在你的眼里是红色的而且模糊不清，这就对了。这就是恒星摇篮，著名的猎户星云。每年一月底二月初晚上八点多的时候，猎户座内连成一线的δ、ε、ζ三颗星正高挂在南天，所以有句民谚说“三星高照，新年来到”。参宿七最佳观测日期为十二月上旬至四月上旬。出现时自东南方升起，经天顶后由西南方落下。猎户座α 及 β 极亮，在一般无云的夜空即可轻易见到，但由于冬季夜空亮星颇多，要辨认出猎户座还须其它星补助，通常利用排成一直线的腰带三星当其辨别指针。此三颗星亮度在 1.7- 2.3 之间，在光害不大的天空易清晰可见，α 及β两星位于腰带之中垂线北南两端，找出后在α的西方及β 的东方再找出 g 及κ两星，整个猎户轮廓已呼之欲出了。观测方位猎户座是冬夜星空中最好认的一个星座（以下是北纬30度地区在不同时间的晚上21时观测到猎户座的方位）日期时间仰角方位每年12月1日 21:00 20-45 东南东每年1月1日 21:00 45-70天顶偏东南每年2月1日 21:00 60-90 天顶偏南每年3月1日 21:00 40-65 西南西每年4月1日 20:00 30-55 西南西语源学和文化意义播报编辑英文语源参宿七的现代名称最早记载于1521年的阿坊欣表（Alphonsine Tables）它来源于阿拉伯语的名字 Rijl Jauzah al Yusrā，即“Jauzah的左腿”（rijl意为“腿，脚”），这个阿拉伯名称可以追溯到10世纪。另一个阿拉伯的名称是رجل الجبار‎ riǧl al-ǧabbār，意思是伟大的一只脚（巨人、征服者），这也是少用到的名称，Algebar或Elgebar，的来源。阿坊欣表（Alphonsine Tables）将参宿七的名字拆成"Rigel"和"Algebar"，并加注解"et dicitur Algebar. Nominatur etiam Rigel."。替换拼字的风潮盛行于17世纪，包括意大利天文学家乔瓦尼·巴蒂斯塔·李却里的Regel，德国天文学家威廉·谢卡特的Riglon，和英国作家和翻译家艾德蒙·Chilmead的Rigel Algeuze 或Algibbar。 [9]欧洲文化参宿七在北欧神话中又称”奥凡迪尔脚趾（Aurvandil's toe）”。 [9]东方和南亚在中国，称为参宿七（Shēnxiù Qī，参宿中的第七颗星）。这个排序与小三星那三颗星有关，最初只有这三颗星，后来添加了四颗星，但原来的名称不变。在日本，源或源氏家族选择参宿七和他的白色作为标志，称这颗星为Genji-boshi (源氏星)；同时平或海克家族以参宿四它的红色为标志。在日本历史中两个强大家族的传奇战争，在天上是指以腰带相隔，对峙的两颗亮星分隔着。参宿七也被称为Gin-waki（银脇），是在美津博世旁边的银色恒星。 [9]新手上路成长任务编辑入门编辑规则本人编辑我有疑问内容质疑在线客服官方贴吧意见反馈投诉建议举报不良信息未通过词条申诉投诉侵权信息封禁查询与解封©2024 Baidu 使用百度前必读 | 百科协议 | 隐私政策 | 百度百科合作平台 | 京ICP证030173号京公网安备110000020000

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Releases: rigelminer/rigel

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满天星斗呼唤我（19）——参宿七 - 知乎

满天星斗呼唤我（19）——参宿七 - 知乎首发于满天星斗呼唤我切换模式写文章登录/注册满天星斗呼唤我（19）——参宿七七小七软件开发行业从业人员之前讲了参宿四的故事，今天就来介绍一下它的小伙伴，参宿七。参宿七，猎户座β，英文名Rigel，光谱类型为B8Ia，又是一颗蓝超巨星（为什么要说又），也是肉眼所见最亮的蓝超巨星。它的目视星等为0.13等，是全天排名第七的亮星。距离我们860光年。老规矩，高清大图奉上作为超巨星，参宿七的质量和体积自然非比寻常。它的半径差不多是太阳的79倍，质量是太阳的21~24倍。表面温度约 12100 K。同之前介绍的天津四一样，它的光度也并不确定，大约在太阳的6万倍~36万倍之间，绝对星等高达-7.84等。在一等星中仅次于天津四。如果把它放在天狼星（8.6光年）的位置上，它的视星等可达到-10等，大约与初八的月亮差不多一样亮。参宿七也是距我们1000光年范围内本质上最亮的恒星。参宿七的年龄只有800万年左右。但对于一颗超巨星来说，这个年龄已经算是暮年了。参宿七在主序星阶段是颗罕见的O型星，表面温度高达 30000K。目前，参宿七已经燃烧尽了核心的氢，温度也下降到之前的一半不到。在它的光谱中可以分辨出氧，镁，钙等元素，这是超巨星光谱的特征之一。参宿七也因此成为了所在光谱类型的分类标准星。读过《三体》的小伙伴们都知道，苦逼的三体星人生活在一个三星系统中。被著名的三体运动问题（三颗恒星互相围绕时运动路径毫无规律）折磨的死去活来，因此才不顾一切的要奔向地球。我们的参宿七身边同样有着一个三合星系统，由三颗主序星参宿七 Ba，参宿七 Bb 与参宿七 C 组成。参宿七 Ba 和参宿七 Bb 是一对分光双星，目视星等为7.5等。之前在介绍角宿一的时候提到过，离的非常近的双星无法在望远镜中区分开来，只能通过光谱来区分它们，这样的双星就叫分光双星。与角宿一一样，参宿七 Ba 和参宿七 Bb 也是双线光谱双星（SB2），这意味着两颗恒星的质量相差不大，分别是太阳的3.84倍和2.94倍。它们表面温度都很高，是光谱类型为B9V的蓝白色主序星，互相围绕旋转一周只需要9.86天。参宿七 C 与参宿七 B 两兄弟一样，也是光谱类型为B9V的蓝白色恒星。它的质量是太阳的3.84倍，目视星等为7.6等。它与参宿七 B 两兄弟相距约30个天文单位，共同构成了一个三星系统，绕行周期为63年。它们三个与参宿七相距2200个天文单位之遥，绕行一周需要24000年。这是一幅三体星的想象图。宇宙中的三合星系统并不罕见，比如我们的老朋友，著名凶星大陵五。不过，像三体星那样的三星系统比较少，大多都是以一对双星+一颗伴星这样的 2+1 的组合存在。参宿七也是一颗变星。不过，它的光度可不像参宿四那样上蹿下跳，它的目视星等变化幅度非常小，在0.05等～0.18等之间变化，偶尔会比御夫座的五车二亮一丢丢，过把第六亮星的瘾，但大多数时候还是牢牢坐稳第七把交椅。参宿七光变周期在几小时到几天不等，并没有明显的规律，属于不规则变星。天文学家把它跟天津四一起归类为“天鹅座α型变星”（参宿七：为什么不叫“猎户座β型变星”？碳基生物：对不起啊，我们是先来后到）。这类变星的光变机制还不大清楚，但成员星都是参宿七这样的蓝超巨星。天鹅座α型变星又叫做非径向脉动变星。变星，就是光度会改变的恒星，是由于某些原因，恒星的大小在不断变化，周期性地膨胀和收缩，导致恒星的亮度也跟着变化。而天鹅座α型变星在以一种很别扭的形式改变形态，某些地方收缩时，某些地方又在扩张。这就导致恒星整体的亮度变化并不明显。相比它话题度爆表的小伙伴参宿四，参宿七就像那种成绩中上的文静学生，自身资质不错，却也达不到惊艳的地步（海山二：咳咳咳，请直接报我名，谢谢），总是安静坐在角落里，不吵不闹（光度相对稳定），受关注程度远远小于光变剧烈，时不时就要"整点活"的参宿四。不过，作为一颗超巨星，参宿七怎么可能是平凡之辈？它在以强烈恒星风的形式不断的抛射物质，并在恒星周围形成了一个气态壳。大概每一百万年就能损失一个太阳的质量。这个损失速度是太阳的1000万倍。从初生到现在，它已经甩掉了差不多3个太阳的质量。我们都知道，质量不同的恒星有着不同的演化路线。对于一颗质量在太阳1~7倍的中等质量的恒星来说，它从主序到暮年，会因为体积膨胀而表面温度下降，从而由高温的蓝/白/黄色变成低温的红色，也就是红巨星。这个过程基本是不可逆的。但是对于超巨星这种top级恒星来说，不整点活怎么能对得起如此庞大的质量呢？超巨星的颜色会根据它不同的发展阶段而反复横跳。从主序到超巨星，基本还是会保持蓝白色，成为一颗蓝超巨星。之后会因体积膨胀，表面温度降低，变成红超巨星。而有的红超巨星会因为爆发等原因，失去表层的物质，重新变成一颗蓝超巨星。我们的参宿七就是这样一个百变boy。根据它的恒星脉动研究表明，它曾经应该变红过，之后因为某种原因，温度升高，又重新变成了蓝超巨星。至于它的未来如何，会不会再来一次川剧变脸，我们还无法得知。不过有一点可以肯定，拥有如此大的质量，参宿七未来一定会发生超新星爆发，化作一朵宇宙烟火，迸发出可以照亮整个银河系的光芒，轰轰烈烈的结束星生。参宿七也是离我们最近的超新星候选星之一。爆发时，参宿七的目视星等将可以达到 -8等 ~ -11等，最亮能跟初九的月亮一样亮。不过，由于距离遥远，并不会对我们产生什么影响。参宿七所在的猎户座，是知名度仅次于北斗七星的著名星座。在全天88个星座中，猎户座以两颗一等星，五颗二等星的豪华阵容排名榜首，是拥有亮星最多，最耀眼的星座。当然，猎户座的牛逼之处还远不止于此。它座内亮于3等的星星几乎全员超巨星。除了左肩的参宿四是红超巨星，其他都是高热的蓝超巨星或蓝巨星。一来，这表明它们都离我们非常远。距离最近的参宿五也在250光年之外。而"腰间佩剑"伐三，距我们约2330光年，是亮于三等的恒星中距离我们最远的一颗。二来，这也意味着猎户座注定是个"短命"的星座。在数千万年内，这些超巨星就会依次变红，爆发，消失，猎户座也终将消失不见。不过，如果我们有穿越时空的能力，就可以在千万年的尺度上，在一个星座里接连见证十几次超新星爆发，想想也是别样的盛况呢。冬季星空最耀眼的星座--猎户座猎户座不止群星闪耀，附近的星云也格外美丽。最有名的应该是猎户座腰间佩剑处的猎户座大星云了。猎户座大星云又叫M42，就位于猎户座腰带三星的左下方。在观测条件好的地方，肉眼就能看见它云雾状的轮廓。当然，在天文摄影大片里能看到肉眼不可见的超震撼细节。它跟仙女座星系常年霸占着天文摄影的热门榜首，也是天文学家最爱的星云之一。猎户座大星云距离我们约1500光年，跨度约40光年。它是一片发光气体云，是新恒星诞生的摇篮，其中大部分恒星的年龄不超过200万~300万年。这片星云中包含了大量的电离氢，暗星云，恒星喷流，它们被新生的炽热恒星照亮，彰显着宇宙的勃勃生机。由NASA拍摄的猎户座大星云，呈现了由氧和氢辐射的辉光著名的马头星云，也位于猎户座之中，就在猎户座大星云的上方。其实它是个范围不大的暗星云，是猎户座分子云的一部分，也距离我们大约1500光年。因外形酷似马的头部而得名。别看它范围不大，却是天文学家和天文摄影爱好者的宠儿，网上的美图一抓一大把。能否找到马头星云，已经成为了业余观星圈内判断望远镜性能好坏和观测者水平的标准之一。暗星云与发射星云，反射星云都不同，是由不发光的弥漫物质所形成的云雾状天体，它们密度很大，足以遮蔽来自背景的星云或恒星的光。暗星云与亮星云交织在一起，为夜空带来了一丝诡谲的色彩。由哈勃望远镜拍摄的马头星云的细节此外，在望远镜的长曝光下，可以看到猎户座被一个巨大的红色新月形星云笼罩着，这就是著名的巴纳德环（Barnard's Loop）。巴纳德环本身是个发射星云。红色是由电离氢产生的。由于过于暗淡，我们肉眼是无法看到的。这片星云的大小和距离还无法确定。根据不同的研究结果，天文学家给出了直径100光年，距离518光年和直径300光年，距离1434光年两组数值。它很可能源于约200万年前的一次超新星爆发（猎户座还真是超新星批发市场啊~）。猎户座与壮观的巴纳德环在上面的图片中，还可以看到右下角参宿七附近，有一片蓝色的星云，这就是著名的女巫头星云了。它的形状很像一个女巫的侧脸（上图中方向不对，要倒过来看才像，如下图），在黑夜里散发出幽幽蓝光，与它的名字很是相衬。女巫头星云是一个反射星云，本身不发光，主要靠反射附近的参宿七的光芒而发光。它的蓝色不止是因为参宿七是蓝白色的。实际上，恒星能发射出所有波段的光，而相对于其他颜色，星云中的气态分子更容易散射蓝色的光，因此反射星云大多都是蓝色的。我们看到天空是蓝色的，是同样的道理。女巫头星云被右上角明亮的参宿七照亮一般说来，星座中最亮的星星会被命名为α星，参宿七是猎户座最亮的恒星，它却并不是猎户座α，而是猎户座β，第二亮的参宿四才是猎户座α。这跟双子座的北河二和北河三是一样的。北河三比北河二更亮，但北河二是双子座α，北河三是双子座β。如此命名的原因众说纷纭。有人说，因为参宿四是著名的变星，光变幅度很大，有时确实比参宿七要亮。也有人觉得，参宿四是明显的黄色，看上去给人的感觉就要比蓝白色的参宿七更明亮一些。还有人认为，它们俩光度本来就差别不大，而参宿四先于地平线升起，所以被命名为α没有毛病。不管怎么说，拜耳给恒星命名的时候，确实没有严格的遵从“谁亮谁老大”的标准，比如天龙座α的亮度只能排到座内第七，但因为是曾经的北极星，地位特殊，便得到了“α星”的名号。参宿四和参宿七错位命名的原因，大概只有拜耳他老人家自己知道啦！猎户座由于过于显眼，不同的文化中都不约而同的把这片天区划为一块。在中国古代的星官体系中，参宿有七颗星，正是猎户座的主体七颗星。参宿七由于在最右下角，就排到了老七的位置。阿拉伯文化中，猎户座则是一个女性的形象。参宿七的英文名Rigel，就来自阿拉伯语短语Rijl Jauzah al Yusrā，意思是"中央腿的左腿"，指的是恒星在猎户座脚或腿上的位置。Jauzah是猎户座的阿拉伯语名称。在日本平安时代的末期（1180年至1185年，南宋高宗时期），两大武士家族，源氏和平氏，发生了著名的源平合战。两大家族都是当时数一数二的贵族，源氏家族选择参宿七和他的白色作为家族标志，称这颗星为Genji-boshi，即源氏星。而平氏家族选择了参宿四和它的红色作为家族标志。两大家族在地上打的不可开交，而在天上，参宿四和参宿七也被腰带三星隔开，在夜空中遥遥对峙，颇具象征意味。这场战争最终以拥有平氏血脉的安德天皇被逼跳海，平氏大败而告终。获胜的源氏首领源赖朝乘胜追击，统一了全日本，在朝廷之下建立了武士政权，史称镰仓幕府，正式拉开了日本长达680年的幕府时代。日本天皇从此成为了吉祥物，直到明治维新，天皇才重新掌权。参宿七也因此格外受到日本的重视，又被称为Gin-waki（银脇），是腰带三星旁边的银色星星的意思。写这篇文章的时候，正是冬夜的晚上。稍微抬头，就能看见参宿七挂在南边的天空中，在低空闪耀着蓝白色的光芒。冬夜的星空实在是太过耀眼，以至于参宿七这样明亮的星星位于其中，都显得有些平平无奇。它与附近的天狼星相比，看上去也确实暗淡了不少。如果不了解它的故事，谁又能想象得到，这是一颗质量是天狼星十几倍，半径是天狼星30多倍的庞然大物呢？星空并不是永恒的，它变化的速度其实比我们想象的还要快。靠近我们的低质量恒星，比如天狼星，织女星，牛郎星，大角，会因为明显的自行，最终远离我们，在百万年的尺度上就会逐渐黯淡。而大质量的恒星，比如天津四，心宿二，参宿四，参宿七，虽然距离遥远，看上去基本不会动，但它们的寿命有限，千万年的尺度上就会爆发，消失在寂寂夜空中。因此，与每一颗恒星的相遇，其实都是难得的缘分，值得我们珍惜和收藏。这也是我写这个专栏的初衷吧。参宿七和女巫头星云。女巫头星云上面就是波江座的起点玉井三专栏目录：满天星斗呼唤我（星星小传）且放远目观玄黄（天文知识小科普）编辑于 2023-09-17 14:09・IP 属地辽宁天文知识天文科普恒星赞同 11458 条评论分享喜欢收藏申请转载文章被以下专栏收录满天星斗呼唤我仰望星空，总想知道每颗星星的名字，每个背后

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Rigel | Blue Supergiant, Orion Constellation & Binary System | Britannica

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Rigel (Beta Orionis) Facts: Size, Mass, Luminosity, Name, Constellation | Star Facts

Rigel (Beta Orionis) Facts: Size, Mass, Luminosity, Name, Constellation | Star Facts Skip to content Star FactsStars: A guide to the night skyHomeBrightest StarsNearest StarsStar NamesTypes of StarsLife Cycle of a StarList of Stars Star FactsStars: A guide to the night sky Navigation Menu Navigation Menu HomeBrightest StarsNearest StarsStar NamesTypes of StarsLife Cycle of a StarList of StarsRigelby admin2019-09-172024-01-24Rigel, Beta Orionis (β Ori), is a blue-white supergiant star located in the constellation Orion, the Hunter. With an apparent magnitude of 0.13, it is the brightest star in Orion and the seventh brightest star in the sky. It is slightly fainter than Vega in the constellation Lyra and Capella in Auriga, but outshines Procyon in Canis Minor, Achernar in Eridanus and (most of the time) its Orion neighbour Betelgeuse. Like Betelgeuse, Rigel is slightly variable, showing fluctuations in brightness from magnitude 0.05 to 0.18. It lies at an estimated distance of 860 light years from Earth.Star systemEven though it appears as a single star to the unaided eye, the Beta Orionis system consists of at least four components, designated Rigel A (or β Ori A), Rigel Ba, Rigel Bb and Rigel C. Rigel B and Rigel C are commonly referred to as Rigel BC. The three fainter components (Rigel Ba, Bb and C) are sometimes simply called Rigel B. There is another star, fainter and at wider separation, that is a suspected component of the system.Rigel A is a luminous supergiant, separated from the fainter triple star system by 9.5 arcseconds. It is 400 times brighter than Rigel BC. Rigel B is a spectroscopic binary star system, which means that its binary nature can only be detected through the stars’ spectral lines because the two components – Rigel Ba and Rigel Bb – are too close together and cannot be resolved visually, even with the largest telescopes. Rigel B and Rigel C, on the other hand, can be resolved, but only with telescopes with very high resolving power.Rigel (Beta Orionis), image: WikiskyRigel BC takes about 24,000 years to complete an orbit around Rigel A, while the components B and C orbit each other with a period of about 63 years. Rigel Ba and Rigel Bb have a considerably shorter period, completing an orbit every 9.860 days.The properties of the components Rigel Ba, Ba and C are difficult to determine because of the stars’ proximity to each other. All three appear to be blue-white main sequence stars of the spectral type B9 V, with similar temperatures. Their estimated masses are also similar at 3.84, 2.94, and 3.84 solar masses respectively.Rigel, as viewed from the Rutherfurd Observatory. Image: Wikimedia Commons/Haktarfone (CC BY-SA 3.0)Rigel ARigel A is a massive, luminous star of the spectral type B8 Ia, indicating a bright supergiant appearing blue or blue-white in colour. The star has a radius almost 79 times that of the Sun and an estimated mass of 21 solar masses. With a temperature of 12,100 K, it shines with about 120,000 solar luminosities. (Its exact luminosity is uncertain, but estimates have been in the range from 61,500 to 363,000 L☉.)Rigel A is classified as an Alpha Cygni variable, which means that, like Deneb (Alpha Cygni), it exhibits small variations in brightness as a result of non-radial pulsations, with some parts of its surface contracting while others simultaneously expand. A number of well-known stars belong to this class, including Alnilam in Orion, Aludra and Omicron2 Canis Majoris in Canis Major, Rho Leonis in Leo, Sigma Cygni in Cygnus, and possibly Naos in Puppis, among others.Rigel has exhausted the supply of hydrogen in its core and, as it evolved from the main sequence, it started to cool and expand to its current size. Based on the star’s pulsations, it is possible that it has already been a blue supergiant once, before evolving into a red supergiant and then increasing its temperature and becoming a blue supergiant again. Even though Rigel’s physical properties are uncertain, the star will face the same fate as other exceptionally massive stars. It will keep fusing increasingly heavier elements in its core until the core can no longer counter gravitational compression and implodes, triggering a Type II supernova.Rigel is one of the nearest known supernova candidates. When it occurs, the supernova will likely reach a visual magnitude of about -11, which is about as bright as a quarter Moon, but it will not affect Earth because the star is too distant.Rigel BRigel B has an apparent magnitude of 6.7, which would make the star easily visible in small telescopes if it were not so close to Rigel A. As it is about 440 times fainter than its neighbour, Rigel B is difficult to see in telescopes with apertures smaller than 6-inch.The binary system is separated from the primary component by 9.5 arcseconds, or more than 2,200 astronomical units. It has a similar proper motion to Rigel A. The two have an orbital period of at least 18,000 years.Rigel B is a double-lined spectroscopic binary (SB2), which means that spectral lines from both stars are visible. Based on the periodic changes in the lines, the two components are believed to have an orbital period of 9.86 days. Both stars are hot and have a spectral classification of about B9. They are believed to form a triple star system with Rigel C.The Gaia Data Release 2 gave a parallax of 2.9186 ± 0.0761 milliarcseconds for Rigel B, which would place the star at an approximate distance of 1,100 light years, or 340 parsecs, from Earth. The distance would be consistent with membership in the Taurus-Orion R1 association, but would place Rigel B considerably further away than Rigel A. However, the Gaia parallax is considered to be unreliable.Rigel CRigel C is separated from Rigel B by less than 0.1 to 0.3 arcseconds. Observations in 2009 revealed that Rigel B and Rigel C had almost identical properties and were separated by only 0.124 seconds of arc. The stars have apparent magnitudes of 7.5 and 7.6 and orbit each other with a period of 63 years.LuminosityRigel is classified as a class Ia luminous supergiant based on its hydrogen spectral lines. With an absolute magnitude of -7.84, if it were located at the same distance from us as Sirius, it would have an apparent magnitude of about -10 and be a little dimmer than the full Moon (mag. -12.74).Even though Rigel is often referred to as the most luminous star within 1,000 light years of Earth, the star’s luminosity is still uncertain. Based on the currently accepted distance of 860 light years, its estimated luminosity is about 120,000 times that of the Sun. However, a recent study gives a distance of 1,170 ± 130 light years, which yields a luminosity of 218,000 solar luminosities.Calculations using stellar evolutionary models give luminosities in the range from 83,000 to 363,000 solar luminosities, while estimates based on angular diameter measurements from the Navy Precision Optical Interferometer, using the Hipparcos distance of 860 light years, indicate an energy output of 61,515 ± 11,486 solar luminosities.BrightnessRigel is usually slightly fainter than Capella, but not always. With Rigel’s brightness varying from magnitude 0.05 to 0.18 and Capella’s from 0.03 to 0.16, Rigel occasionally outshines Auriga’s brightest star, briefly becoming the sixth brightest star in the sky.Rigel’s variability has been known since at least 1930. However, the variations in the star’s brightness have a small amplitude and can only be detected photoelectrically or with CCD photometry. The variations do not have a clear period. A study conducted in 1984 revealed variations of up to 0.13 magnitudes over several hours to a few days, but with no apparent period.In 1998, a study of B stars observed with the Hipparcos satellite presented a classification of new variable stars discovered by Hipparcos and classified Rigel as an Alpha Cygni variable. Alpha Cygni stars generally seem to have irregular variations because they are caused by pulsations, which can appear irregular because there are multiple pulsation periods, typically lasting from several days to several weeks. The mechanism of pulsations is not entirely understood.MassRigel’s mass is also uncertain. A comparison of evolutionary tracks yielded a mass of 21 ± 3 solar masses at an age of 8 ± 1 million years. However, calculations based on atmospheric modelling from the star’s spectrum produced a value of 24 ± 8 solar masses.Rigel’s H-alpha emissions show a P Cygni profile, a spectroscopic feature that indicates the existence of an expanding shell of gas and a dense stellar wind, both associated with mass loss. However, the star shows a P Cygni profile only a quarter of the time and its line profiles transform every few days, sometimes indicating mass loss and at other times infalling material. The changes have been explained as a result of varying quantity and velocity of the material lost from the star. A study published in 1997 suggests that the changes are due to Rigel having extended rotating magnetic structures emerging from its photosphere.Based on observations of Rigel’s variable H-alpha line, the star is estimated to lose mass at a rate of (1.5 ± 0.4) × 10−7 solar masses per year, or 10 million times faster than the Sun. Later studies gave a mass loss rate of (9.4 ± 0.9) × 10−7 solar masses per year (2006-2007) and (7.6 ± 1.1) × 10−7 solar masses per year (2009-2010), based on observations of Rigel’s H-gamma line. Rigel is believed to have lost about 3 solar masses from its initial mass of 24 ± 3 solar masses, which it had when it began its life 7 to 9 million years ago.ColourLike all class B supergiants, Rigel is very luminous and appears distinctly bluish in colour, in stark contrast to the red supergiant Betelgeuse.Rigel serves as a spectral standard for its class, B8 Ia. Its spectrum shows neutral helium lines and strong hydrogen absorption lines, characteristic of its class, as well as heavier elements, including oxygen, magnesium and calcium.Photo taken by Rogelio Bernal Andreo in October 2010 of the Orion constellation showing the surrounding nebulae of the Orion Molecular Cloud Complex. Also captured is the red supergiant Betelgeuse (top left) and the famous belt of Orion composed of the OB stars Alnitak, Alnilam and Mintaka. Rigel can be found at the bottom right. The red crescent shape is Barnard’s Loop. Image: Rogelio Bernal Andreo (CC BY-SA 3.0)DistanceRigel’s currently accepted distance from the Sun is about 863 light years, or 265 parsecs, based on the 2007 Hipparcos reduction of the star’s parallax (3.78 ± 0.34 milliarcseconds). The margin of error is about 9%.However, the Gaia Data Release 2 gave a parallax of 2.9186 ± 0.0761 milliarcseconds for one of Rigel’s fainter companions, which translates into a distance of 1,100 light years, or 340 parsecs. As the companion is a close binary system, the value may not be reliable.Rigel’s distance has also been estimated through indirect measurements. The star illuminates the nearby Witch Head Nebula (IC 2118), which extends for about 5 degrees at an angular separation of 2.5 degrees (or 39 light-years) from the star. Distance measurements of the stars embedded within the nebula yielded a value of 949 ± 7 light-years, or 291 ± 2 parsecs.Supergiant Rigel and IC 2118 in Eridanus, image: European Southern Observatory, credit: Robert Gendler (CC BY 4.0)SizeThe measurements of Rigel’s angular diameter and size have also produced different results. An older value given for the star’s angular diameter is 2.75 ± 0.01 milliarcseconds, which translates into a radius 78.9 times solar. However, a study published in 2017 that used the Navy Precision Optical Interferometer to measure the star’s apparent size gave a value of 2.526 milliarcseconds for Rigel’s angular diameter and derived a radius of 74.1 solar radii (allowing for a margin of error in the range from 66.8 to 80.2 solar radii), close to the orbit of Mercury.UY Scuti compared to other stars, image: Wikimedia Commons/IStoleThePies (CC BY-SA 4.0)TemperatureRigel’s estimated surface temperature is around 12,100 K based on the star’s colour and spectral class. That’s less than 50% compared to its temperature before it evolved off the main sequence (about 30,000 K).FactsRigel has the Bayer designation Beta Orionis even though most of the time it is brighter than Betelgeuse, which got the designation Alpha. This is not the only case of the brightest star in a constellation not being designated Alpha (e.g. the brightest stars in Sagittarius, Ursa Major, Pegasus, Hercules and Gemini have the designations Epsilon Sagittarii, Epsilon Ursae Majoris, Epsilon Pegasi, Beta Herculis, and Beta Geminorum). However, it is possible that when German uranographer Johann Bayer assigned Greek letters to stars around the year 1600, Betelgeuse was in fact brighter than Rigel. Bayer was guided by magnitude class, not the exact order of brightness, and did not use the same scheme for every constellation, so it is also possible that he used a different logic when assigning the letters to Orion stars.Rigel is one of the 58 stars selected by Her Majesty’s Nautical Almanac Office and the US Naval Observatory for navigation. It is one of four navigational stars in Orion. The other three are Betelgeuse and Bellatrix, the bright stars marking Orion’s shoulders, and Alnilam, the central star of Orion’s Belt.Rigel has been known to be a multiple star system for several centuries. The German-born British astronomer William Herschel discovered it to be a double star on October 1, 1781. He entered it as star 33 (H II 33) in his Catalogue of Double Stars.In 1871, American astronomer Sherburne Wesley Burnham suspected Beta Orionis B to be a binary star and was able to resolve it into two stars in 1878. The second star is now designated as Rigel C. Burnham entered Rigel as β 555 (the modern BU 555) in his catalogue of double stars.In 1878, Burnham also observed another suspected companion, a 13th magnitude star, and catalogued it as component D of β 555. The star was separated by 44.5 arcseconds from Rigel in 2007. Whether or not it is a member of the Beta Orionis system is still uncertain. The Gaia Data Release 2 identified it as a sun-like star, likely an orange dwarf, of 12th magnitude, located at about the same distance as Rigel. If it is a member of the Rigel star system, its estimated orbital period would be about 250,000 years.Rigel is considered to be a member of the Taurus-Orion R1 Association, a loose group of stars that share a common origin and motion through space, located about 1,200 light years, or 360 parsecs, from the solar system. Some sources classify the star as an outlying member of the Orion OB1 association, but since Rigel is much closer to us than the stars in the Orion OB1 group, lying at a similar distance as Betelgeuse and Saiph, its membership is unlikely.Variations in Rigel’s radial velocity (the speed at which it moves relative to Earth) were first detected in 1888 and later confirmed to vary by about 10 km/s.In images of the Orion constellation, Rigel is commonly depicted as the foot of Orion. The nearby Cursa, Beta Eridani, represents Orion’s footstool.Like many other exceptionally bright stars, Rigel had cultural and historic significance in many countries around the world. In Japan, it was chosen to represent the Genji clan, one of the four major clans during the Heian period (794-1185). They called the star Genji-boshi (源氏星). The rivalling Taira clan chose Betelgeuse and its red colour as their symbol. The two clans fought the Genpei War and Rigel and Betelgeuse were seen as facing off against each other in the sky, with only the Orion’s Belt stars keeping them apart. Rigel was also called Gin-waki (銀脇), meaning “the silver star beside Mitsu-boshi (Orion’s Belt).”Rigel may be the star marking “Orwandil’s toe” in Norse mythology. In the myth, Orwandil, the Giant, was frostbitten and Thor broke off his frozen toe and threw it into the sky. Since the broken off toe is more commonly associated with Alcor in Ursa Major, Richard Hinckley Allen suggests that Alcor is the frost-bitten toe and Rigel, the other toe in his Star Names: Their Lore and Meaning (1889).In Caribbean lore, Rigel marked the severed leg of Trois Rois, a man who loved the daughter of a woman who disliked him. As the lovers took flight, the mother ran after them and managed to cut off one of his legs. The daughter is represented by Aldebaran, Trois Rois by the stars of Orion’s Belt, and the mother by Sirius.Two places in Antarctica were named after Rigel: the Rigel Skerries and Mount Rigel.Rigel has been used in countless works of fiction, including multiple episodes of Star Trek and the films Star Trek: The Motion Picture (1979) and Fantastic Four: Rise of the Silver Surfer (2007). Notable uses of the star in literature include M. A. R. Barker’s Tékumel novels and games, the novels Next of Kin (1959) by Eric Frank Russell, Jack Vance’s Demon Princes series (1964-1981), and Timothy Zahn’s Night Train to Rigel (2005).NameThe name Rigel (pronunciation: /ˈraɪdʒəl/) comes from the Arabic phrase Rijl Jauzah al Yusrā, meaning “the left leg of the central one,” and refers to the star’s position at the foot or leg of Orion. Jauzah was the Arabic name for the constellation Orion, representing a female figure whose identity is uncertain.The less common names for the star were Algebar or Elgebar, derived from the Arabic riǧl al-ǧabbār, meaning “the foot of the great one.” The name Rigel was also spelled as Regel, Riglon, Algibbar and Rigel Algeuze.The name dates back to the 10th century. The earliest known written mention of it is in the Alfonsine Tables of 1521.The International Astronomical Union’s (IAU) Working Group on Star Names (WGSN) officially approved the name Rigel for Beta Orionis A on June 30, 2016. Even though the name formally applies only to the brightest component, it is commonly used for the entire star system and its individual components.Rigel has been known by many different names across different cultures. The Chinese know it as the Seventh Star of Three Stars, referring to the Chinese Three Stars (參宿) asterism, which originally consisted of the three stars of Orion’s Belt, but was later expanded to include four other bright stars of Orion.The Lacandon people of Mexico called the star tunsel, meaning “the little woodpecker.”The Wotjobaluk koori of Victoria in Australia knew Rigel as Yerrerdet-kurrk. It represented the mother-in-law of Totyerguil, marked by Altair. The distance between the two stars symbolized the taboo of a man approaching his mother-in-law.The Boorong people of Victoria called the star Collowgullouric Warepil, while the Wardaman people of the Northern Territory knew it as the Red Kangaroo Leader Unumburrgu, who led ceremonies when the constellation was high in the sky. The other bright stars of Orion represented his tools and followers.The Māori people of New Zealand knew the star as Puanga, a daughter of Rehua, the chief of all stars, represented by Antares. Rigel’s heliacal rising heralded the appearance of the Pleiades, known as Matariki, in the morning sky in late May or early June, symbolizing the Māori New Year.LocationRigel is easy to find because it is part of one of the most recognizable constellations in the sky. Marking the left foot of Orion, the star appears as the bottom right star of Orion’s hourglass figure to northern observers and as the top left star to observers in the southern hemisphere.Orion stars, image: WikiskyRigel marks one of the vertices of the Winter Hexagon (or Winter Circle), a large asterism that dominates the evening sky during the northern hemisphere winter. Other vertices of the Winter Hexagon are at Aldebaran in Taurus, Capella in Auriga (which is part of a smaller hexagon formed by the brightest stars in Auriga and Elnath in Taurus), Pollux in Gemini, Procyon in Canis Minor and Sirius in Canis Major, the brightest star in the sky.The Winter Triangle and the Winter Hexagon, image: WikiskyRigel is located in the vicinity of several notable deep sky objects. The nearest one is the Witch Head Nebula (IC 2118), a faint reflection nebula illuminated by Rigel, located in the region between Rigel and Cursa, in the neighbouring constellation Eridanus. The faint H II region Sharpless 278 lies just north of Rigel. The Orion Nebula (Messier 42), which lies a bit further away and appears as the central star of Orion’s Sword, forms a triangle with Rigel and Saiph, Orion’s other foot.Rigel, the Orion Nebula and the Witch Head Nebula, image: WikiskyRigel can be seen from all locations on Earth except those within 8 degrees of the North Pole. It is at its highest point in the sky at midnight on December 12 and at 9 pm on January 24. The best time of year to see Rigel and other stars in Orion is during the month of January, when the constellation is prominent in the evening sky. From northern locations, Rigel is visible from late summer to early spring at some point in the night.As the name implies, this reflection nebula associated with the star Rigel looks suspiciously like a fairytale crone. Formally known as IC 2118 in the constellation Orion, the Witch Head Nebula glows primarily by light reflected from the star. The color of this very blue nebula is caused not only by blue color of its star, but also because the dust grains reflect blue light more efficiently than red. A similar physical process causes Earth’s daytime sky to appear blue. Image: NASA/STScI Digitized Sky Survey/Noel CarboniConstellationRigel is located in the constellation Orion, the Hunter. Named after the Greek mythical hunter, Orion is one of the most conspicuous constellations in the sky. Rigel marks the giant huntsman’s left foot, possibly the one stung by the scorpion in the myth, outlining the constellation’s hourglass figure with six other bright stars: Betelgeuse and Bellatrix marking the shoulders, Alnitak, Alnilam and Mintaka forming the Belt of Orion, and Saiph marking the other foot.Orion constellation map by IAU and Sky&Telescope magazineThe constellation is known for its two familiar asterisms, Orion’s Belt and Orion’s Sword. Orion’s Sword contains the bright, large Orion Nebula (M42) with the young Trapezium Cluster, the neighbouring De Mairan’s Nebula (M43), and the Running Man Nebula (Sharpless 279). Orion is also home to the reflection nebulae Messier 78 and NGC 1999, the dark Horsehead Nebula, and the emission nebulae NGC 2174 (the Monkey Head Nebula), NGC 2024 (the Flame Nebula), and Barnard’s Loop (Sharpless 276).Orion dominates the evening sky from January to March. The 10 brightest stars in the constellation are Rigel (Beta Ori, mag. 0.05 – 0.18), Betelgeuse (Alpha Ori, mag. 0.0 – 1.3), Bellatrix (Gamma Ori, mag. 1.59 to 1.64), Alnilam (Epsilon Ori, mag. 1.64 – 1.74), Alnitak A (Zeta Ori A, mag. 2.00), Saiph (Kappa Ori, mag. 2.09), Mintaka AB (Delta Ori AB, mag. 2.23), Hatysa (Iota Ori, mag. 2.77), Tabit (Pi3 Ori, mag. 3.16), and Eta Orionis (mag. 3.31 – 3.6).Rigel – Beta OrionisAbsolute magnitude-7.84Distance860 ± 80 light years (260 ± 20 parsecs)Parallax3.78 ± 0.34 masRadial velocity17.8 ± 0.4 km/sProper motionRA: +1.31 mas/yrDec.: +0.50 mas/yrConstellationOrionDesignationsRigel, Beta Orionis, β Ori, ADS 3823, H II 33, BU 555, STF 668, WDS J05145-0812, CCDM J05145-0812Rigel ASpectral classB8 IaVariable typeAlpha CygniU-B colour index-0.66B-V colour index-0.03Apparent magnitude0.13 (0.05 – 0.18)Mass21 ± 3 M☉Luminosity120,000 L☉ (99,000 – 145,000 L☉)Radius78.9 ± 7.4 R☉Temperature12,100 ± 150 KMetallicity−0.06 ± 0.10Age8 ± 1 million yearsRotational velocity25 ± 3 km/sSurface gravity1.75 ± 0.10 cgsRight ascension05h 14m 32.27210sDeclination-08° 12′ 05.8981”Designations19 Orionis, HR 1713, HD 34085, HIP 24436, FK5 194, BD-08°1063, SAO 131907, CSV 100463, GC 6410, GCRV 3110, IRAS 05121-0815, AAVSO 0509-08, 2MASS J05143226-0812060, PPM 187839, TYC 5331-1752-1Rigel BCSpectral classB9V + B9VApparent magnitude6.67 (7.5/7.6)Mass (Rigel Ba, Bb, C)3.84 M☉, 2.94 M☉, 3.84 M☉Right ascension05h 14m 32.049sDeclination-08° 12′ 14.78”Designations (Rigel B)Rigel B, GCRV 3111Tags:AchernarAlcorAldebaranAlnilamAlnitakAlpha CygniAlpha OrionisAludraAntaresBellatrixBeta EridaniBeta GeminorumBeta HerculisBeta OrionisBetelgeuseCapellaCursaDenebElnathEpsilon PegasiEpsilon SagittariiEpsilon Ursae MajorisIC 2118Messier 42MintakaNaosOmicron-2 Canis MajorisOrion NebulaOrion OB1 AssociationOrion's BeltOrion's SwordP CygniPleiadesPolluxProcyonRho LeonisRigelRigel ARigel BRigel CSaiphSharpless 278Sigma CygniSiriusTaurus-Orion R1 AssociationVegaWinter CircleWinter HexagonWitch Head Nebula Search for... 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Rigel: Orion's Brightest Star

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By Elizabeth Howell published 18 March 2019

Reference Article

Light from the star Rigel reflects off the dust composing the Witch Head Nebula.

(Image credit: Rogelio Bernal Andreo / NASA)

Rigel is a blue supergiant that is the brightest star in the constellation Orion (the Hunter). Due to its measured size and brightness it is expected to end in a supernova one day. It also has two known companions, Rigel B and Rigel C.The star is about 870 light-years from the sun and 47,000 times as luminous, according to Encyclopedia Britannica. It is a variable star (its apparent brightness varies) and is considered an Alpha Cygni-type star. Alpha Cygni is the scientific name for Deneb, the prototype star for this kind of brightness variability. Rigel's name is popular in science-fiction. It's in the name of a number of planets in the "Star Trek" universe, is mentioned in "The Hitchhiker's Guide to the Galaxy," and is also featured in a number of other novels, computer games and comic books.The name comes from an Arabic phrase, "Rijl Jauzah al Yusrā," which means, "The left leg of the Jauzah," according to Richard Hinckley Allen's book "Star Names: Their Lore and Meaning" (Dover Publications, 2013). The phrase is also sometimes translated as "The left leg of the giant," referring to the constellation Orion, which Rigel is a part of. Rigel is more properly (to astronomers) known as Beta Orionis.Locating RigelRigel is close to zero magnitude in Earth's sky, making it a bright star, and is best visible in the winter northern sky. Rigel's location is:Right ascension: 5 hours 14 minute 32.3 secondsDeclination: -8 degrees 12 minutes 6 secondsRigel has two distant stellar companions, Rigel B and Rigel C — a binary system. At the ninth magnitude, the combined light of these stars would usually be enough for most telescopes to pick up, but they are too close to Rigel to be distinguished apart.Rigel's bright starlight also bounces off a nearby nebula, as shown in a picture published in 2012 on NASA's Astronomy Picture of the Day website.A view of the winter night sky showing where the constellation Orion will be visible. [Full story] (Image credit: Starry Night)"The blue color of the Witch Head Nebula and of the dust surrounding Rigel is caused not only by Rigel's intense blue starlight, but because the dust grains scatter blue light more efficiently than red," NASA wrote. "The same physical process causes Earth's daytime sky to appear blue, although the scatterers in Earth's atmosphere are molecules of nitrogen and oxygen."Astronomers have made several observations of Rigel in recent years. For example, a 2014 study examined the variability of stellar winds coming from Rigel over several years. The astronomers noted that the observations were made in high spatial and spectral resolution. And, a 2017 study measured the stellar flux density of Rigel and two other stars, Aldebaran and Fomalhaut. Stellar flux refers to how much radiation energy a star emits. In general, the group found that stellar flux density is at a minimum at the outer surface of a star and at a maximum inside of the star.Due to its proximity, Rigel is also used as an example of how massive stars may evolve, as discussed in a 2013 review published by the European Astronomical Society, and a 2014 study published in the Proceedings of the International Astronomical Union.Additional resources: Find out How the Night Sky Constellations Got Their Names. Learn why astrology is not a science. Check out NASA's star image gallery at Hubblesite.

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Betelgeuse and Rigel: A tale of the two brightest stars in Orion

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By Joe Rao published 18 March 2021

Betelgeuse and Rigel are two bright stars in the constellation of Orion, the hunter. (Image credit: Starry Night)This week, the grandest and most spectacular of all constellations can be found due south and standing upright around 7 p.m. local time, and dominating our winter skies like — to use the words of astronomer Robert H, Baker — "a gigantic piece of jewelry." It's the "great hunter" or "celestial warrior," Orion, the most brilliant of the constellations and visible from every inhabited part of the Earth. As is also the case with the mighty Hercules, the figure of Orion has been associated in virtually all ancient cultures with great national heroes, warriors or demigods. Yet, in contrast to Hercules, who was credited with a detailed series of exploits, Orion seems to us a vague and shadowy figure. The ancient mythological stories of Orion are so many and so confused that it is almost impossible to choose among all of them. Even the origin of the name Orion is obscure, though some scholars have suggested a connection with the Greek "Arion," meaning "warrior." All, however, agree that he was the mightiest hunter in the world, and he is always pictured in the stars with his club upraised in his right hand. Hanging from his upraised left hand is the skin of a great lion he has killed and which he is brandishing in the face of Taurus, the bull, who is charging down upon him. Related: Exploring Orion's wonders using mobile astronomy apps Shining down upon us through the frosty air all winter long, three bright stars in a diagonal line in the middle of a bright rectangle decorate Orion's belt, which points northward to the star clusters of the Hyades and Pleiades in Taurus, and southward to the brightest of all stars, the "Dog Star" Sirius. Polar opposites

Within Orion we find two immense stars, Rigel and Betelgeuse, apparently at diametrically opposite periods in a star's existence. In Rigel (the "left leg of the giant"), we find a star apparently reaching the prime of its life. It is the seventh-brightest star in our sky and is a true supergiant: a blazing blue-hot star of intense brilliance and dazzling beauty, one of the rarest breeds in our galaxy. Located 863 light-years away, Rigel's computed luminosity is an incredible 120,000 times the brightness of our sun. Its surface temperature is also far hotter than the sun, around 21,000 degrees Fahrenheit (11,600 degrees Celsius). Compare that to 10,000 degrees F (5,500 degrees C) for the sun. In terms of overall size, Rigel measures 79 times the diameter of the sun. And yet, it's only 21 times more massive. This sky map shows where you can see the Orion constellation, Mars and two star clusters (the Pleiades and Hyades) in the night sky. (Image credit: SkySafari app)In stark contrast, Betelgeuse (the "armpit" of the giant), shines with a cool, dull ruddy hue and is located 548 light-years away, though there is an uncertainty of as much as 100 light-years with this figure. Like Rigel, Betelgeuse's luminosity far exceeds that of our sun. It is an irregular pulsating supergiant star, nearing the end of its life and as such it expands and contracts spasmodically. Incredibly, its diameter can vary between 550 to 920 times the diameter of our sun, meaning that at its maximum size, were it placed at the center of our solar system, it would engulf the planets Mercury, Venus, Earth, Mars and Jupiter. In trying to describe Betelgeuse some three-quarters of a century ago, Henry Neeley, a long-time lecturer at New York's Hayden Planetarium noted that it is "like an old man with his strength almost entirely spent, panting in the asthmatic decrepitude of old age."An unexpected eclipse

Betelgeuse was much in the news at this time last year, because it was undergoing an unusual dimming. Because of its irregular pulsations, it was well known that Betelgeuse could appear to noticeably brighten and fade over time. But a year ago, it had diminished to magnitude +1.6. Normally the tenth-brightest star in the sky, within a matter of just a few months Betelgeuse had fallen to the rank of a second-magnitude star (if rounded off to the nearest whole magnitude). There was much speculation that this anomalous dimming was a sign that the star might be preparing to end its life as a supernova. But by the spring of 2020, the star had once again reverted back to its "normal" brightness of magnitude +0.4. It has since faded somewhat again, though nothing to compare to the drastic fade down of a year ago. Gesundheit!

So, what was the reason for the "Betelgeuse brownout?" On Aug. 13, 2020, the Harvard Smithsonian Center for Astrophysics released a statement attributing the fade-down of Betelgeuse as a "stellar sneeze." The star's fade-down was "most likely caused by the ejection and cooling of dense hot gases, and that the star may be going through another dimming period more than a year early," according to the statement. The gas and dust that was blown away after the "big sneeze" eventually condensed into a dark cloud. That cloud blocked a part of the star's face as seen from the perspective of Earth and thus caused the star to appear to dim. Some residual gas and dust may have since condensed into a smaller cloud which may be resulting in another round of apparent dimming of Betelgeuse at the present time.Bang!

Stars produce their energy by fusing hydrogen into helium deep within their cores. When a star accumulates sufficient helium in its core, its energy output increases significantly, and it swells into a red giant or supergiant, like Betelgeuse. This is what Rigel will become in a few million years. In such stars, the core produces successively heavier elements to balance the incessant crush of gravity. But once the core begins creating iron, a star's days are numbered; the formation of elements heavier than iron consumes rather than produces energy. Eventually, since the core can no longer support the star's vast weight it collapses, triggering a cataclysmic supernova explosion. Betelgeuse is in its final stage and could explode within the next 100,000 years.Joe Rao serves as an instructor and guest lecturer at New York's Hayden Planetarium. He writes about astronomy for Natural History magazine, the Farmers' Almanac and other publications. Follow us on Twitter @Spacedotcom and on Facebook.

Join our Space Forums to keep talking space on the latest missions, night sky and more! And if you have a news tip, correction or comment, let us know at: community@space.com.

Joe RaoSocial Links NavigationSkywatching ColumnistJoe Rao is Space.com's skywatching columnist, as well as a veteran meteorologist and eclipse chaser who also serves as an instructor and guest lecturer at New York's Hayden Planetarium. He writes about astronomy for Natural History magazine, the Farmers' Almanac and other publications. Joe is an 8-time Emmy-nominated meteorologist who served the Putnam Valley region of New York for over 21 years. You can find him on Twitter and YouTube tracking lunar and solar eclipses, meteor showers and more. To find out Joe's latest project, visit him on Twitter.

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