Formation of Globular Clusters in Galaxies

星系中球状星团的形成

• 批准号: 04452013
• 负责人: FUJIMOTO Mitsuaki
• 金额: $ 4.54万
• 依托单位: Nagoya University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (B)
• 财政年份: 1992
• 资助国家: 日本
• 起止时间: 1992 至 1993
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-04452013/
• 关键词: globular clusters; galaxies; gravitational instability; binary clusters; 回転; 星団形成; 重力不安定; 二重球状星団

We made a model for the orbits of the Large and Small Magellanic Clouds (LMC and SMC) to reproduce the density and velocity destribution of hydrogen gas in the Magellanic stream. In the successful model LMC and SMC from a gravitationally bound pair and have revolved around the Galaxy over the past - 10^<10> y. They exprienced a close encounter every - 10^9 y and have been agitated by tidal force repeatedly to keep the interstellar gas turbulent with the turbulent velocity higher than (〕SY.gtoreq.〔) 50 km s^<-1>.Turbulent eddies (gas clouds) collide with each other frequently and form compressed gas layers at the interfaces. The compressed gas layrs rotate and have internal velocity shear because the collisions are usually off-center and rarely head-on. Our linear stability analysis showed that the compressed gas layrs fragment into gravitationally bound clumps with the mass of 10^4 - 10^6 M_<(〕SY.sun.〔)> after it grows in mass and its self-gravity becomes appreciable. The gaseous clumps cool rapidly due to their high density and cascade into much smaller fragments, finally froming gravitationally-bound stellar systems or globular clusters.We thus conclude that globular clusters are not cosmological objects formed only in the early universe but ordinary ones formed at any epoch in the galaxies in which a large amount of interstellar gas has an unorganized motion with the velocity higher than 50 km s^<-1>. The color, age, and mass distributions of globular clusters manifest the history of the dynamical events experienced by the host galaxy.

我们为大型和麦哲伦云（LMC和SMC）的轨道制作了一个模型，以在成功的LMC和SMC中从一个重力中复制氢的密度和破坏。过去-10> y。他们遇到了近距离的ternar turberent。在界面上形成压缩气体层。 6 m _ <（] sysun。[）>在质量生长后，自我验证是可观的。不是仅形成Y宇宙，而是在星系中形成的任何时代，以速度大的速度，超过50 m s^<-1>的速度。主机银河系经历的动态事件的历史。

项目成果

T.Hanawa: "Effects of Magnetic Field and Rotation on the Fragmentation of Filamentary Molecular Clords:Comparison of the Theory with the Orion A Cloud" Astrophys.J.Letters. 404. L86-L89 (1992)

T.Hanawa：“磁场和旋转对丝状分子团碎片的影响：该理论与猎户座 A 云的比较”Astrophys.J.Letters。

Y.Kumai: "Formation of Globular Clusters from Gas in Large-Scale Unorganized Motion in Galaxies." Astrophys.J.404. 114-161 (1993)

Y.Kumai：“星系中大规模无组织运动中气体形成球状星团。”

G.T.Gardiner: "Numerical Simulation of the Magellanic Stream. I." Monthly Notices of Royal Astoronomical Society. 266. 567-582 (1994)

G.T.Gardiner：“麦哲伦流的数值模拟。I。”

Y.Kumai: "Formation of Globular Clusters from Gas in Large-Scale Unorganized Motion in Galaxies" Astrophysical Journal. 404. 144-161 (1993)

Y.Kumai：“星系中大规模无组织运动中气体形成球状星团”天体物理学杂志。

T.Hanawa: "Effects of Magnetic Field and Rotation on the Fragmentation of Filamentary Molecular Clouds : Comparison of the Theory with the Orion A Cloud." Astrophys.J.Letters. 404. L86-L89 (1992)

T.Hanawa：“磁场和旋转对丝状分子云破碎的影响：该理论与猎户座 A 云的比较。”