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Revised rates for the stellar triple-alpha process from measurement of C-12 nuclear resonances

Fynbo, H. O. U. (author)
Århus Universitet,Aarhus University
Diget, C. A. (author)
Århus Universitet,Aarhus University
Bergmann, U. C. (author)
Organisation européenne pour la recherche nucléaire (CERN),European Organization for Nuclear Research (CERN)
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Borge, M. J. G. (author)
CSIC - Instituto de Estructura de la Materia (IEM)
Cederkall, J. (author)
Organisation européenne pour la recherche nucléaire (CERN),European Organization for Nuclear Research (CERN)
Dendooven, P. (author)
Fraile, L. M. (author)
Organisation européenne pour la recherche nucléaire (CERN),European Organization for Nuclear Research (CERN)
Franchoo, S. (author)
Organisation européenne pour la recherche nucléaire (CERN),European Organization for Nuclear Research (CERN)
Fedosseev, V. N. (author)
Organisation européenne pour la recherche nucléaire (CERN),European Organization for Nuclear Research (CERN)
Fulton, B. R. (author)
University of York
Huang, W. X. (author)
Jyväskylän Yliopisto,University of Jyväskylä
Huikari, J. (author)
Jyväskylän Yliopisto,University of Jyväskylä
Jeppesen, H. B. (author)
Århus Universitet,Aarhus University
Jokinen, A. S. (author)
Helsingin Yliopisto,University of Helsinki,Jyväskylän Yliopisto,University of Jyväskylä
Jones, P. (author)
Jyväskylän Yliopisto,University of Jyväskylä
Jonson, Björn, 1941 (author)
Chalmers tekniska högskola,Chalmers University of Technology
Koster, U. (author)
Organisation européenne pour la recherche nucléaire (CERN),European Organization for Nuclear Research (CERN)
Langanke, K. (author)
Århus Universitet,Aarhus University
Meister, Mikael, 1969 (author)
Chalmers tekniska högskola,Chalmers University of Technology
Nilsson, Thomas, 1965 (author)
Chalmers tekniska högskola,Chalmers University of Technology
Nyman, Göran Hugo, 1943 (author)
Chalmers tekniska högskola,Chalmers University of Technology
Prezado, Y. (author)
CSIC - Instituto de Estructura de la Materia (IEM)
Riisager, K. (author)
Århus Universitet,Aarhus University
Rinta-Antila, S. (author)
Jyväskylän Yliopisto,University of Jyväskylä
Tengblad, O. (author)
CSIC - Instituto de Estructura de la Materia (IEM)
Turrion, M. (author)
CSIC - Instituto de Estructura de la Materia (IEM)
Wang, Y. B. (author)
Jyväskylän Yliopisto,University of Jyväskylä
Weissman, L. (author)
Organisation européenne pour la recherche nucléaire (CERN),European Organization for Nuclear Research (CERN)
Wilhelmsen, Katarina, 1962 (author)
Chalmers tekniska högskola,Chalmers University of Technology
Aysto, J. (author)
Jyväskylän Yliopisto,University of Jyväskylä,Helsingin Yliopisto,University of Helsinki
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 (creator_code:org_t)
Springer Science and Business Media LLC, 2005
2005
English.
In: Nature. - : Springer Science and Business Media LLC. - 0028-0836 .- 1476-4687 .- 1476-4679. ; 433:7022, s. 136-139
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http://dx.doi.org/10...
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  • Journal article (peer-reviewed)
Abstract Subject headings
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  • In the centres of stars where the temperature is high enough, three alpha-particles (helium nuclei) are able to combine to form C-12 because of a resonant reaction leading to a nuclear excited state(1). (Stars with masses greater than similar to0.5 times that of the Sun will at some point in their lives have a central temperature high enough for this reaction to proceed.) Although the reaction rate is of critical significance for determining elemental abundances in the Universe(1), and for determining the size of the iron core of a star just before it goes supernova(2), it has hitherto been insufficiently determined(2). Here we report a measurement of the inverse process, where a C-12 nucleus decays to three alpha-particles. We find a dominant resonance at an energy of similar to11 MeV, but do not confirm the presence of a resonance at 9.1 MeV (ref. 3). We show that interference between two resonances has important effects on our measured spectrum. Using these data, we calculate the triple-a rate for temperatures from 10(7) K to 10(10) K and find significant deviations from the standard rates(3). Our rate below similar to5 x 10(7) K is higher than the previous standard, implying that the critical amounts of carbon that catalysed hydrogen burning in the first stars are produced twice as fast as previously believed(4). At temperatures above 10(9) K, our rate is much less, which modifies predicted nucleosynthesis in supernovae(5,6).

Subject headings

NATURVETENSKAP  -- Fysik -- Subatomär fysik (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Subatomic Physics (hsv//eng)

Keyword

PARTICLES
B-12
BETA-DECAY
NUCLEOSYNTHESIS
ELEMENTS
ASTROPHYSICS
STARS

Publication and Content Type

art (subject category)
ref (subject category)

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