A star cluster in which hundreds of thousands to millions of stars are densely packed in a spherical shape in an area of about 100 to 300 light years. The density of stars increases rapidly toward the center. Globular clusters are distributed in the halo of the Milky Way, wrapping around the Galactic disk, and are thought to have formed in the early stages of the formation of the Milky Way. The nearest one is about 7,000 light years from Earth, and the farthest is about 350,000 light years away. They are made up of Population II stars, and the amount of heavy elements is less than 10% of that of the Sun, with many even being less than 1%. In globular clusters, the short-lived blue main sequence stars have already evolved, so in the HR diagram (color-magnitude diagram), the main sequence is only redder than G-type stars, and it smoothly connects to the red giant branch. In addition, a horizontal branch consisting of stars evolved from red giants is also clearly visible. In recent years, observations of globular clusters in galaxies other than the Milky Way have also progressed. The distance of a galaxy can also be estimated from the luminosity function of a globular cluster. The population density, color distribution, and other properties of globular clusters in galaxies other than the Milky Way can differ from those in the Milky Way, suggesting that the process by which globular clusters form varies from galaxy to galaxy. [Okamura Sadanori] [References] | | | | |A globular cluster in the constellation Aquarius. NGC7089. Photographed using the Murikabushi Telescope at Ishigakijima Astronomical Observatory © National Astronomical Observatory of Japan "> M2 globular cluster A globular cluster in the constellation Hercules. NGC6205. Also known as the Great Globular Cluster of Hercules. ©National Astronomical Observatory of Japan "> M13 globular cluster A globular cluster in the constellation Pegasus. NGC7078. Photographed using the Murikabushi Telescope at Ishigakijima Astronomical Observatory ©National Astronomical Observatory of Japan "> M15 globular cluster A globular cluster in the constellation Tucana. NGC104 ©ESA/Hubble(Davide De Martin),the ESA/ESO/NASA Photoshop FITS Liberator&Digitized Sky Survey 2 "> Tucanae 47 Source: Shogakukan Encyclopedia Nipponica About Encyclopedia Nipponica Information | Legend |
数十万から百万個程度の星が100から300光年程度の領域に球状に密集している星団。中心に行くほど星の密度が急速に高くなる。球状星団は、銀河系のハロー内に銀河系円盤(ディスク)を包み込むように分布していて、銀河系のできる初期に形成された天体と考えられている。もっとも近いもので地球から約7000光年、もっとも遠いものは約35万光年も離れている。種族Ⅱの星からなり、重元素量は太陽の10%以下で1%以下のものも多い。球状星団では、寿命の短い青い主系列星はすでに進化してしまっているので、HR図(色‐等級図)では、主系列はG型星程度より赤い部分しかなく、それが赤色巨星分枝へと滑らかにつながっている。また、赤色巨星より進化した星からなる水平分枝も顕著に見られる。近年は、銀河系以外の銀河の球状星団の観測も進んでいる。球状星団の光度関数から銀河の距離を推定することもできる。銀河系以外の銀河にある球状星団の個数密度や色分布などの性質は、銀河系のものとは異なる場合があり、球状星団のできるプロセスは銀河によって異なることが示唆されている。 [岡村定矩] [参照項目] | | | | |みずがめ座にある球状星団。NGC7089。石垣島天文台むりかぶし望遠鏡により撮影©国立天文台"> M2球状星団 ヘルクレス座にある球状星団。NGC6205。ヘルクレス座大球状星団ともよばれる©国立天文台"> M13球状星団 ペガスス座にある球状星団。NGC7078。石垣島天文台むりかぶし望遠鏡により撮影©国立天文台"> M15球状星団 きょしちょう座にある球状星団。NGC104©ESA/Hubble(Davide De Martin),the ESA/ESO/NASA Photoshop FITS Liberator&Digitized Sky Survey 2"> きょしちょう座47 出典 小学館 日本大百科全書(ニッポニカ)日本大百科全書(ニッポニカ)について 情報 | 凡例 |
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