Difference between revisions of "Generalized Nucleosynthesis in a Massive Star"
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| − | + | |name=Generalized Nucleosynthesis in a Massive Star | |
| − | + | |next=Portion of Electromagnetic Spectrum Related to Earth and Space Sciences | |
| − | [[File:Generalized Nucleosynthesis in a Massive Star.png|800px]] | + | |desc=Generalized Nucleosynthesis in a Massive Star from the NYS Earth and Space Sciences Reference Tables (ESSRT): the fusion stages from hydrogen to iron in a massive star and how long each one lasts, down to core collapse. Supports HS-ESS1-3. |
| + | }} | ||
| + | The '''Generalized Nucleosynthesis in a Massive Star''' model from the ''Reference Tables for Earth and Space Sciences'' (ESSRT) shows the series of nuclear fusion stages that build heavier and heavier elements inside a massive star, and how long each stage lasts. It primarily supports [[HS-ESS1-3]]. | ||
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| + | [[File:Generalized Nucleosynthesis in a Massive Star.png|800px|class=img-fluid|alt=Generalized Nucleosynthesis in a Massive Star from the Earth and Space Sciences Reference Tables (ESSRT): cross section of a massive star with fusion shells from hydrogen to iron around an iron core, and a table of how long each stage lasts]] | ||
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| + | == What the nucleosynthesis model shows == | ||
| + | The model is drawn as a cross section of the star, with fusion shells layered like an onion: hydrogen fusing to helium in the outermost shell, then helium to carbon, carbon to oxygen, oxygen to silicon and silicon to iron, around a core of iron (Fe). A table beside it gives the duration of each stage: 7 × 10<sup>6</sup> years for hydrogen to helium, 7 × 10<sup>5</sup> years for helium to carbon, 600 years for carbon to oxygen, 6 months for oxygen to silicon, 1 day for silicon to iron and a quarter of a second for core collapse. Each stage is far shorter than the one before it. | ||
Latest revision as of 13:05, 13 October 2026
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The Generalized Nucleosynthesis in a Massive Star model from the Reference Tables for Earth and Space Sciences (ESSRT) shows the series of nuclear fusion stages that build heavier and heavier elements inside a massive star, and how long each stage lasts. It primarily supports HS-ESS1-3.
What the nucleosynthesis model shows
The model is drawn as a cross section of the star, with fusion shells layered like an onion: hydrogen fusing to helium in the outermost shell, then helium to carbon, carbon to oxygen, oxygen to silicon and silicon to iron, around a core of iron (Fe). A table beside it gives the duration of each stage: 7 × 106 years for hydrogen to helium, 7 × 105 years for helium to carbon, 600 years for carbon to oxygen, 6 months for oxygen to silicon, 1 day for silicon to iron and a quarter of a second for core collapse. Each stage is far shorter than the one before it.