Photonuclear Reactions in Astrophysics
Photonuclear Reactions in Astrophysics
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DOI：
10.1080/10619127.2018.1463016
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发表时间：
2018-03
影响因子：
--
通讯作者：
T. Rauscher
中科院分区：
文献类型：
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作者：
T. Rauscher
恒星的核合成和恒星爆炸是通过热化等离子体中的核反应进行的。核反应不仅使元素及其同位素发生嬗变，从而从原始氢和氦中创造出所有已知的元素，它们还释放出能量，使恒星在天文时间尺度上保持流体静力平衡。恒星等离子体必须足够热，以提供足够的动能给等离子体成分，以克服库仑势垒，并允许它们之间的相互作用。处于热平衡的等离子体成分是裸露的原子核、自由电子和光子（辐射）。经历核燃烧的等离子体的典型温度范围从107 K的流体静力学氢燃烧（主要是质子和He同位素之间的相互作用）到1010 K或更高的爆炸事件，如超新星或中子星星合并。根据核物理学标准，这仍然转化为低相互作用能量，因为反应伙伴之间在温度方面的最可能能量E来自麦克斯韦-玻尔兹曼统计，并产生E = T9/11.6045 MeV，其中T9是GK的等离子体温度。
Nucleosynthesis in stars and stellar explosions proceeds via nuclear reactions in thermalized plasmas. Nuclear reactions not only transmutate elements and their isotopes, and thus create all known elements from primordial hydrogen and helium, they also release energy to keep stars in hydrostatic equilibrium over astronomical timescales. A stellar plasma has to be hot enough to provide sufficient kinetic energy to the plasma components to overcome Coulomb barriers and to allow interactions between them. Plasma components in thermal equilibrium are bare atomic nuclei, free electrons, and photons (radiation). Typical temperatures of plasmas experiencing nuclear burning range from 107 K for hydrostatic hydrogen burning (mainly interactions among protons and He isotopes) to 1010 K or more in explosive events, such as supernovae or neutron star mergers. This still translates into low interaction energies by nuclear physics standards, as the most probable energy E between reaction partners in terms of temperature is derived from Maxwell-Boltzmann statistics and yields E = T9/11.6045 MeV, where T9 is the plasma temperature in GK.