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Volumn 299, Issue 5603, 2003, Pages 70-75

Genesis of the heaviest elements in the milky way galaxy

Author keywords

[No Author keywords available]

Indexed keywords

ASTROPHYSICS; CHEMICAL ELEMENTS; HEAVY METALS; NEUTRON SOURCES; THORIUM;

EID: 0037414870     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.1077506     Document Type: Review
Times cited : (83)

References (38)
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    • The high temperatures that would be required (to overcome the electric Coulomb barriers) for fusion of nuclei beyond iron would also result in a large number of high-energy photons. These photons in turn result in photodisintegration of nuclei that suppress any possible charge-particle fusion reactions.
  • 3
    • 0346945095 scopus 로고    scopus 로고
    • note
    • H fusion in stars occurs in the inner core (approximately the innermost 10% of the star by mass) and lasts for about 90% of the star's total life. After the exhaustion of H in the core, the star will then develop a thin (thousands of km) H fusion shell outside of the inert He core. Later, when the temperature rises to above 100 million K, the He core will fuse C and O. When the He is finally depleted in the core, a thin He fusion shell, outside of the now C/O core but interior to the H fusion shell, will ignite. These later fusion stages occur only during the last ∼10% of a star's life.
  • 4
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    • note
    • Supernovae (SNe) are observationally categorized by the presence (type II) or absence (type I) of hydrogen spectral lines. Further, type II SNe are normally thought to result from the collapse and explosion of single massive, short-lived stars. Type I SNe are thought to be phenomena of lower-mass, longer-lived binary star systems, with the eventual explosion and complete destruction of the white dwarf member of the binary.
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    • C. A. Barnes, D. D. Clayton, D. N. Schramm, Eds. (Cambridge Univ. Press, Cambridge
    • A. G. W. Cameron, in Essays in Nuclear Astrophysics, C. A. Barnes, D. D. Clayton, D. N. Schramm, Eds. (Cambridge Univ. Press, Cambridge, 1982), pp. 23-43.
    • (1982) Essays in Nuclear Astrophysics , pp. 23-43
    • Cameron, A.G.W.1
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    • note
    • Caution is recommended in interpreting the r-process fractions of isotopes with extreme dominance by the s-process: A small error (∼10%) in the s-process fraction in these cases leads to a large uncertainty (≥25%) in the remainder r-process fraction.
  • 10
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    • note
    • sun]. With this definition [Fe/H] is normally used as a surrogate for overall metallicity, and for example [Eu/Fe] tells the difference in stellar and solar Eu/Fe abundance ratios.
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    • R. Cayrel et al., Nature 409, 691 (2001).
    • (2001) Nature , vol.409 , pp. 691
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    • note
    • We thank our colleagues for helpful conversations and insightful comments, and P. Möller for providing us with a copy of Fig. 1. Supported by NSF grants AST-9987162 (C.S.) and AST-9986974 (J.J.C.), Space Telescope Science grant GO-08342, and the University of Texas at Austin Department of Astronomy John W. Cox Fund (J.J.C.).


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.