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Determination of Key Nuclear Reaction Rates Governing 44Ti Production in Core Collapse Supernovae

Determination of Key Nuclear Reaction Rates Governing 44Ti Production in Core Collapse Supernovae
核心塌陷超新星中控制 44Ti 产生的关键核反应速率的确定
批准号:
EP/D032288/1
负责人:
Alexander Murphy
金额:
$16.29万
依托单位:
依托单位国家:
英国
项目类别:
Research Grant
财政年份:
2006
资助国家:
英国
项目状态:
已结题
起止时间:
2006 至 --

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Where does the calcium in your teeth and your bones come from? How can the same material in far off galaxies be used to understand the biggest explosions in the Universe? You might be surprised to know! Billions of years ago a star, a bit larger than our Sun, ended its life in an explosion so powerful it would have briefly been as bright as all the other stars in our Galaxy put together. In that explosion, known as a supernova, many of the elements that we are made of will have been created. As this material expanded and cooled it will have formed into dust, spreading out through space. From this dust, the Earth, the Sun and all the rest of our solar system has formed. As the Nobel laureate William Fowler said, 'All of us are truly and literally a little bit of stardust'. One of the elements created is the metal titanium, and a certain type of this, known as titanium-44, changes into calcium through a natural process called radioactive beta decay. As we look out into space today, we can occasionally see supernovae occurring in other Galaxies, or sometimes even our own (the last one that we know of occurred in 1667). Satellites orbiting the Earth can look at these in great detail. One of the things they hope to see is titanium-44 changing into calcium. They can see this because when this transition occurs very energetic particles of light, called gamma-rays, are emitted, making it visible even over the vast distances involved. Moreover, we can work out how many gamma rays were emitted, and we can use that as a test of computer models of what we think is happening to make the stars explode in the first place. Even our best models, running on some of the world's most powerful computers, still have great difficulty in simulating these events, and so tests such as this or of great current need. Some of the most important things we yet need to know to make these simulations sufficiently accurate, are what are known as nuclear reaction rates. Just as the calcium is
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45 V ( p , ? ) thermonuclear reaction rate relevant to 44 Ti production in core-collapse supernovae: General estimates and shell model analysis
与核心塌陷超新星中 44 Ti 产生相关的 45 V ( p , ? ) 热核反应速率:一般估计和壳模型分析
DOI: 10.1103/physrevc.66.015801
发表时间: 2002
期刊: Physical Review C
影响因子: 3.1
作者: [Horoi M]
通讯作者: Horoi M
The 45V(p,?) thermonuclear reaction rate relevant to 44Ti production rate in core-collapsed supernovae: a shell model analysis
核心塌陷超新星中与 44Ti 生成速率相关的 45V(p,?) 热核反应速率:壳模型分析
DOI: 10.1016/s0375-9474(03)00870-4
发表时间: 2003
期刊: Nuclear Physics A
影响因子: 1.4
作者: [Horoi M]
通讯作者: Horoi M
BRIdging Disciplines of Galactic Chemical Evolution (BRIDGCE) Consortium 2021-2024
  • 批准号:
    ST/V000462/1
  • 项目类别:
    Research Grant
  • 资助金额:
    $2.88万
  • 财政年份:
    2021
  • 负责人:
    Alexander Murphy
  • 依托单位:
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    ST/V001809/1
  • 项目类别:
    Research Grant
  • 资助金额:
    $3.88万
  • 财政年份:
    2021
  • 负责人:
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  • 依托单位:
XENON FUTURES: R&D for a Global Rare Event Observatory - Phase 1
  • 批准号:
    ST/T005874/1
  • 项目类别:
    Research Grant
  • 资助金额:
    $0.9万
  • 财政年份:
    2019
  • 负责人:
    Alexander Murphy
  • 依托单位:
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  • 批准号:
    ST/M003744/1
  • 项目类别:
    Research Grant
  • 资助金额:
    $3.9万
  • 财政年份:
    2015
  • 负责人:
    Alexander Murphy
  • 依托单位:
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βB1 蛋白 L116P 突变通过 Greek key II 的稳定 性介导晶状体蛋白异常聚集的作用与机制研 究
  • 批准号:
    Q24H120009
  • 项目类别:
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    2024
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    LY23H120004
  • 项目类别:
    省市级项目
  • 资助金额:
    --
  • 批准年份:
    2023
  • 负责人:
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  • 依托单位:
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  • 项目类别:
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  • 资助金额:
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  • 批准年份:
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  • 负责人:
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