Helium destruction and gamma-ray line emission in accreting neutron stars
Helium destruction and gamma-ray line emission in accreting neutron stars
复制标题
吸积中子星中的氦破坏和伽马射线线发射
DOI：
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发表时间：
1993
期刊：
影响因子：
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通讯作者：
I. Wasserman
中科院分区：
文献类型：
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作者：
L. Bildsten;E. Salpeter;I. Wasserman
中子星星的普遍伽马射线生产渠道-从中子-质子复合的2.2 MeV的光子的发射-被重新考虑。计算了2.2MeV γ射线线通量和康普顿散射连续谱。来自最明亮的吸积X射线源天蝎座X-1的引力红移2.2 MeV光子的通量约为10 exp-6伽马/平方厘米s，比康普顿伽马射线天文台的灵敏度低20倍。吸积He-4的破坏导致高层大气中较轻元素（D，H-3，He-3）的显着丰度，这是确定的。被摧毁的He-4在光球层下几个尺度的高度通过聚变反应重新形成，因此不会阻碍H射线爆发。
The prevalent gamma-ray production channel of a neutron star - emission of 2.2-MeV photons from neutron-proton recombination - is reconsidered. The 2.2-MeV gamma-ray line flux and Compton-scattered continuum are calculated. The flux of gravitationally redshifted 2.2-MeV photons from the brightest accreting X-ray source Scorpius X-1 is about 10 exp -6 gamma/sq cm s, a factor of 20 below the sensitivities on the Compton Gamma-Ray Observatory. The destruction of accreted He-4 leads to significant abundances of lighter elements (D, H-3, He-3) in the upper atmosphere, which are determined. The destroyed He-4 is reformed through fusion reactions a few scale heights beneath the photosphere, and thus does not hamper H-ray bursts.