dc.citation.endPage |
399 |
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dc.citation.number |
2 |
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dc.citation.startPage |
389 |
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dc.citation.title |
ASTROPHYSICAL JOURNAL |
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dc.citation.volume |
354 |
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dc.contributor.author |
Ryu, Dongsu |
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dc.contributor.author |
Vishniac, Ethan T. |
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dc.contributor.author |
Chiang, Wei-Hwan |
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dc.date.accessioned |
2023-12-22T13:09:15Z |
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dc.date.available |
2023-12-22T13:09:15Z |
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dc.date.created |
2015-08-27 |
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dc.date.issued |
1990-05 |
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dc.description.abstract |
The evolution and distribution of the intergalactic medium (IGM) in a universe dominated by cold dark matter with Omega(0) = 1 and h = 0.5 are investigated. Galaxies form and eject energy into the IGM from z about 20 up to the present, and the distribution of the IGM is dominated by large connected structures. The power spectrum and two-point correlation function of the IGM show a suppressed growth due to the energy injected from galaxies and the mass subtraction to form galaxies. The high-temperature regions of the IGM correspond to the low-density regions and the low-temperature regions correspond to the high-density regions. The temperature of the IGM increases from z = 1 to z = 0, while the prsssure decreases. The present temperature distribution shows a peak at about 10 million K. The mass fraction of the IGM with temperature below 100,000 K is negligible, indicating almost all the hydrogen is ionized. |
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dc.identifier.bibliographicCitation |
ASTROPHYSICAL JOURNAL, v.354, no.2, pp.389 - 399 |
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dc.identifier.doi |
10.1086/168700 |
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dc.identifier.issn |
0004-637X |
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dc.identifier.scopusid |
2-s2.0-4244099368 |
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dc.identifier.uri |
https://scholarworks.unist.ac.kr/handle/201301/18566 |
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dc.identifier.url |
http://adsabs.harvard.edu/doi/10.1086/168700 |
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dc.identifier.wosid |
A1990DC92700001 |
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dc.language |
영어 |
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dc.publisher |
IOP PUBLISHING LTD |
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dc.title |
A MODEL FOR THE DISTRIBUTION OF THE INTERGALACTIC MEDIUM |
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dc.type |
Article |
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dc.description.journalRegisteredClass |
scopus |
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