Thermal and Dynamical Evolution of Primordial Gas Clouds. On the Formation of First Luminous Objects.
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- Nishi Ryoichi
- Department of Physics, Kyoto University, Kyoto 606–8502, Japan
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- Susa Hajime
- Center for Computational Physics, University of Tsukuba Tsukuba 305–8571, Japan
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- Uehara Hideya
- Division of Theoretical Astrophysics, National Astronomical Observatory Mitaka 181–8588, Japan
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- Yamada Masako
- Department of Physics, Kyoto University, Kyoto 606–8502, Japan
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- Omukai Kazuyuki
- Department of Physics, Kyoto University, Kyoto 606–8502, Japan
書誌事項
- タイトル別名
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- Thermal and Dynamical Evolution of Prim
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We investigate the thermal and dynamical evolution of primordial gas clouds in the universe after decoupling. Comparing the time scale of dynamical evolution with that of fragmentation, we can estimate the typical fragmentation scale. We propose the following scenario of the formation process of first luminous objects consisting of large number stars. First, by pancake collapse of the overdensity regions in the expanding universe or collision between clouds in potential wells, quasi-plane shocks form. If the shock-heated temperature is higher than about 104 K, the post-shock gas cools down to several hundred K by H2 line cooling, and the shock-compressed layer fragments into filamentary clouds. The filamentary cloud collapses dynamically once more and fragments into cloud cores. Finally, a primordial star forms in a cloud core. We show that the minimum mass of the first star is essentially determined by the it Chandrasekhar mass . Also, we investigate the dynamical collapse of cloud cores by numerical simulation and show that the evolution paths of the central regions of the cores depend only very weakly on the total core mass. After mass accretion, a massive star may be formed in a core, since the estimated mass accretion rate is very large. In such a case, it may be possible for many massive stars form almost simultaneously. Then the clouds can be luminous objects. On the other hand, if the shock-heated temperature is lower, effective star formation is delayed significantly.
収録刊行物
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- Progress of Theoretical Physics
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Progress of Theoretical Physics 100 (5), 881-903, 1998
一般社団法人 日本物理学会
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詳細情報 詳細情報について
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- CRID
- 1390001204157234304
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- NII論文ID
- 110001200698
- 210000110255
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- NII書誌ID
- AA00791455
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- BIBCODE
- 1998PThPh.100..881N
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- ISSN
- 13474081
- 0033068X
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- NDL書誌ID
- 4616000
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- 本文言語コード
- en
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- データソース種別
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- JaLC
- NDL
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- CiNii Articles
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- 使用不可