Massive star evolution: Nucleosynthesis and nuclear reaction rate uncertainties

A. Heger; S. E. Woosley; T. Rauscher; R. D. Hoffman; M. M. Boyes

doi:10.1016/S1387-6473(02)00184-7

Massive star evolution: Nucleosynthesis and nuclear reaction rate uncertainties

A. Heger, S. E. Woosley, T. Rauscher, R. D. Hoffman, M. M. Boyes

Research output: Contribution to journal › Short Survey › Research › peer-review

21 Citations (Scopus)

Abstract

We present a nucleosynthesis calculation of a 25 M_⊙ star of solar composition that includes all relevant isotopes up to polonium. We follow the stellar evolution from hydrogen burning till iron core collapse and simulate the explosion using a 'piston' approach. We discuss the influence of two key nuclear reaction rates, ¹²C(α, γ)¹⁶O and ²²Ne(α, n)²⁵Mg, on stellar evolution and nucleosynthesis. The former significantly influences the resulting core sizes (iron, silicon, oxygen) and the overall presupernova structure of the star. It thus has significant consequences for the supernova explosion itself and the compact remnant formed. The later rate considerably affects the s-process in massive stars and we demonstrate the changes that different currently suggested values for this rate cause.

Original language	English
Pages (from-to)	463-468
Number of pages	6
Journal	New Astronomy Reviews
Volume	46
Issue number	8-10
DOIs	https://doi.org/10.1016/S1387-6473(02)00184-7
Publication status	Published - 1 Jan 2002
Externally published	Yes

Keywords

Nuclear physics: uncertainties
Stars: massive, evolution, nucleosynthesis

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10.1016/S1387-6473(02)00184-7

Cite this

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title = "Massive star evolution: Nucleosynthesis and nuclear reaction rate uncertainties",

abstract = "We present a nucleosynthesis calculation of a 25 M⊙ star of solar composition that includes all relevant isotopes up to polonium. We follow the stellar evolution from hydrogen burning till iron core collapse and simulate the explosion using a 'piston' approach. We discuss the influence of two key nuclear reaction rates, 12C(α, γ)16O and 22Ne(α, n)25Mg, on stellar evolution and nucleosynthesis. The former significantly influences the resulting core sizes (iron, silicon, oxygen) and the overall presupernova structure of the star. It thus has significant consequences for the supernova explosion itself and the compact remnant formed. The later rate considerably affects the s-process in massive stars and we demonstrate the changes that different currently suggested values for this rate cause.",

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AU - Heger, A.

AU - Woosley, S. E.

AU - Rauscher, T.

AU - Hoffman, R. D.

AU - Boyes, M. M.

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N2 - We present a nucleosynthesis calculation of a 25 M⊙ star of solar composition that includes all relevant isotopes up to polonium. We follow the stellar evolution from hydrogen burning till iron core collapse and simulate the explosion using a 'piston' approach. We discuss the influence of two key nuclear reaction rates, 12C(α, γ)16O and 22Ne(α, n)25Mg, on stellar evolution and nucleosynthesis. The former significantly influences the resulting core sizes (iron, silicon, oxygen) and the overall presupernova structure of the star. It thus has significant consequences for the supernova explosion itself and the compact remnant formed. The later rate considerably affects the s-process in massive stars and we demonstrate the changes that different currently suggested values for this rate cause.

AB - We present a nucleosynthesis calculation of a 25 M⊙ star of solar composition that includes all relevant isotopes up to polonium. We follow the stellar evolution from hydrogen burning till iron core collapse and simulate the explosion using a 'piston' approach. We discuss the influence of two key nuclear reaction rates, 12C(α, γ)16O and 22Ne(α, n)25Mg, on stellar evolution and nucleosynthesis. The former significantly influences the resulting core sizes (iron, silicon, oxygen) and the overall presupernova structure of the star. It thus has significant consequences for the supernova explosion itself and the compact remnant formed. The later rate considerably affects the s-process in massive stars and we demonstrate the changes that different currently suggested values for this rate cause.

KW - Nuclear physics: uncertainties

KW - Stars: massive, evolution, nucleosynthesis

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VL - 46

SP - 463

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JO - New Astronomy Reviews

JF - New Astronomy Reviews

IS - 8-10

ER -

Massive star evolution: Nucleosynthesis and nuclear reaction rate uncertainties

Abstract

Keywords

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