The spectra of X-ray bursting neutron stars
The spectra of X-ray bursting neutron stars
复制标题
X射线爆发中子星的光谱
DOI：
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发表时间：
1984
期刊：
影响因子：
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通讯作者：
R. Taam
中科院分区：
文献类型：
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作者：
R. London;W. M. Howard;R. Taam
我们提出了X射线爆发中子星的自洽大气模型，其中包括非弹性康普顿散射和自由-自由和束缚-自由的发射和吸收的影响。我们表明，计算的光谱比黑体的有效温度相同。这种光谱硬化效应是由于电子散射减少了辐射源函数，以及自由-自由不透明度的强频率依赖性。使用计算出的光谱来解释观测结果在较低的辐射热表面通量比已推断出的黑体发射在有效温度的共同假设。因此，从观测到的光谱温度推断的表观超爱丁顿通量可能会产生误导，除非有精确的距离测定。铁吸收功能的预期强度和它们的使用作为诊断的引力红移在中子星星表面进行了讨论。
We present self-consistent atmospheric models for X-ray bursting neutron stars which include the effects of inelastic Compton scattering and free-free and bound-free emission and absorption. We show that the calculated spectra are harder than blackbodies of the same effective temperature. This spectra hardening effect is attributable to the reduction of the radiation source function by electron scattering, and the strong frequency dependence of the free-free opacity. Using the calculated spectra to interpret the observations results in lower bolometric surface fluxes than has been inferred from the common assumption of blackbody emission at the effective temperature. The apparent super-Eddington fluxes inferred from observed spectral temperatures can thus be misleading unless accurate distance determinations are available. The expected strength of iron absorption features and their use as diagnostics for the gravitational redshift at the neutron star surface are also discussed.