Reionization scenarios and the temperature of the intergalactic medium
Reionization scenarios and the temperature of the intergalactic medium
复制标题
再电离情景和星系间介质的温度
DOI：
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发表时间：
2006
期刊：
影响因子：
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通讯作者：
A. Meiksin
中科院分区：
文献类型：
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作者：
E. Tittley;A. Meiksin
我们使用与粒子网格(PM)N体程序相耦合的辐射转移(RT)程序来研究由于单个电离锋面的通过而引起的IGM的温度结构。对不同的电离辐射光谱进行了多次模拟：幂定律(/o i 0.5)、迷你星体、星暴，以及从星暴光谱演变为幂定律的时变光谱。RT在时间和空间上有足够的分辨率，可以正确地模拟电离状态和电离前沿的温度。我们发现，再电离星系间介质(IGM)的电离后温度对电离辐射源的光谱很敏感，这可能被用来对再电离源的性质施加强烈的限制。辐射传输效应也会导致HeII与HI数密度比的大幅波动。除了随时间变化的频谱外，数值上的差异比测量的要小。在这种情况下，传播演变为光谱性质。
We examine the temperature structure of the IGM due to the passage of individual ionisation fronts using a radiative transfer (RT) code coupled to a particle-mesh (PM) N-body code. Multiple simulations were performed with different spectra of ionising radiation: a power law (/ o i0.5 ), miniquasar, starburst, and a time-varying spectrum that evolves from a starburst spectrum to a power law. The RT is sufficiently resolved in time and space to correctly model both the ionisation state and the temperature across the ionisation front. We find the post-ionisation temperature of the reionised intergalactic medium (IGM) is sensitive to the spectrum of the source of ionising radiation, which may be used to place strong constraints on the nature of the sources of reionisation. Radiative transfer effects also produce large fluctuations in the HeII to HI number density ratio ´. The spread in values is smaller than measured, except for the time-varying spectrum. For this case, the spread evolves as the spectral nature “