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

Author

Listed:
  • Hans O. U. Fynbo

    (University of Aarhus)

  • Christian Aa. Diget

    (University of Aarhus)

  • Uffe C. Bergmann

    (CERN)

  • Maria J. G. Borge

    (Instituto Estructura de la Materia, CSIC, Serrano 113bis)

  • Joakim Cederkäll

    (CERN)

  • Peter Dendooven

    (KVI, Zernikelaan)

  • Luis M. Fraile

    (CERN)

  • Serge Franchoo

    (CERN)

  • Valentin N. Fedosseev

    (CERN)

  • Brian R. Fulton

    (University of York)

  • Wenxue Huang

    (University of Jyväskylä)

  • Jussi Huikari

    (University of Jyväskylä)

  • Henrik B. Jeppesen

    (University of Aarhus)

  • Ari S. Jokinen

    (University of Jyväskylä
    University of Helsinki)

  • Peter Jones

    (University of Jyväskylä)

  • Björn Jonson

    (Experimental Physics, Chalmers University of Technology and Göteborg University)

  • Ulli Köster

    (CERN)

  • Karlheinz Langanke

    (University of Aarhus)

  • Mikael Meister

    (Experimental Physics, Chalmers University of Technology and Göteborg University)

  • Thomas Nilsson

    (CERN)

  • Göran Nyman

    (Experimental Physics, Chalmers University of Technology and Göteborg University)

  • Yolanda Prezado

    (Instituto Estructura de la Materia, CSIC, Serrano 113bis)

  • Karsten Riisager

    (University of Aarhus)

  • Sami Rinta-Antila

    (University of Jyväskylä)

  • Olof Tengblad

    (Instituto Estructura de la Materia, CSIC, Serrano 113bis)

  • Manuela Turrion

    (Instituto Estructura de la Materia, CSIC, Serrano 113bis)

  • Youbao Wang

    (University of Jyväskylä)

  • Leonid Weissman

    (CERN)

  • Katarina Wilhelmsen

    (Experimental Physics, Chalmers University of Technology and Göteborg University)

  • Juha Äystö

    (University of Jyväskylä
    University of Helsinki)

  • The ISOLDE Collaboration

    (CERN)

Abstract

Stellar performance In 1953 Fred Hoyle predicted that in the extreme conditions prevailing in the centre of stars, three α-particles (helium nuclei) can combine to form an excited form of carbon-12. This type of stellar nucleosynthesis is now recognized as the source of heavy elements in the Universe. Surprisingly there is still considerable uncertainty about the nature of the reaction that produces carbon-12. Fynbo et al. have now obtained a much more accurate measure of the reaction rate for carbon-12 synthesis than previously available, by measuring the reverse reaction rate. At temperatures found in young stars the new reaction rate is roughly twice the previous value, but at the 109 K found in supernovae, nucleosynthesis is much slower than was thought.

Suggested Citation

  • Hans O. U. Fynbo & Christian Aa. Diget & Uffe C. Bergmann & Maria J. G. Borge & Joakim Cederkäll & Peter Dendooven & Luis M. Fraile & Serge Franchoo & Valentin N. Fedosseev & Brian R. Fulton & Wenxue , 2005. "Revised rates for the stellar triple-α process from measurement of 12C nuclear resonances," Nature, Nature, vol. 433(7022), pages 136-139, January.
    • Handle: RePEc:nat:nature:v:433:y:2005:i:7022:d:10.1038_nature03219
    DOI: 10.1038/nature03219
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