End point of the rp process on accreting neutron stars.
End point of the rp process on accreting neutron stars.
复制标题
吸积中子星 rp 过程的终点。
DOI：
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发表时间：
2001
影响因子：
8.6
通讯作者：
M. Wiescher
中科院分区：
文献类型：
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作者：
H. Schatz;A. Aprahamian;V. Barnard;L. Bildsten;A. Cumming;M. Ouellette;T. Rauscher;F. Thielemann;M. Wiescher
我们计算了氢在吸积中子星星表面燃烧的快速质子（rp）捕获过程，并更新了反应网络，扩展到1000，远远超过了以前的工作。在这两个稳定状态的核燃烧适合于快速吸积中子星（如磁极帽吸积的X射线恒星）和不稳定燃烧的I型X射线爆发，我们发现，RP过程结束于一个封闭的SnSbTe循环。这阻止了比Te重的元素的合成，并对x射线暴剖面、吸积中子星的组成和潜在的轻p核的星系核合成产生重要影响。
We calculate the rapid proton ( rp) capture process of hydrogen burning on the surface of an accreting neutron star with an updated reaction network that extends up to Xe, far beyond previous work. In both steady-state nuclear burning appropriate for rapidly accreting neutron stars (such as the magnetic polar caps of accreting x-ray pulsars) and unstable burning of type I x-ray bursts, we find that the rp process ends in a closed SnSbTe cycle. This prevents the synthesis of elements heavier than Te and has important consequences for x-ray burst profiles, the composition of accreting neutron stars, and potentially galactic nucleosynthesis of light p nuclei.