薄和细长吸积盘中的垂直耗散廓线和光球位置
Vertical dissipation profiles and the photosphere location in thin and slim accretion disks
摘要：
我们计算光学厚，但几何薄（和超薄）吸积盘模型和执行的光子（在克尔几何）的射线追踪计算所观察到的磁盘光谱。以前，通常的做法是假设光子是从克尔几何赤道平面z = 0发射的，来进行光线跟踪。我们表明，与此假设计算的光谱不同的假设下，光子是从光盘的实际表面发射，z = H（r）的计算。这意味着薄盘有效光球的位置的知识是相关的计算光谱。在本文中，我们调查，在一个简单的玩具模型，可能的影响（未知的，因此特设假设）的垂直耗散配置文件上的垂直结构的磁盘，从而对有效光球的位置，并对所观察到的光谱。对于中等和高质量吸积率（\dot m>0.01 \dot m_C）的磁盘，我们发现，光球的位置在内部，辐射压力为主，磁盘区域（其中大部分的辐射来自）不依赖于耗散配置文件，因此新兴的磁盘光谱是不敏感的耗散函数的选择。对于较低的吸积率光球的位置取决于假设的垂直耗散轮廓下到磁盘的内边缘，但依赖性是非常弱的，因此是次要的。我们的结论是，光学厚吸积盘周围的黑洞的光谱应该计算与射线跟踪从有效光球，幸运的是，一个特定的垂直耗散配置文件的选择并没有实质上影响计算的光谱。
英文摘要：
We calculate optically thick but geometrically thin (and slim) accretion disk models and perform a ray-tracing of photons (in the Kerr geometry) to calculate the observed disk spectra. Previously, it was a common practice to ray-trace photons assuming that they are emitted from the Kerr geometry equatorial plane, z = 0. We show that the spectra calculated with this assumption differ from these calculated under the assumption that photons are emitted from the actual surface of the disc, z = H(r). This implies that a knowledge of the location of the thin disks effective photosphere is relevant for calculating the spectra. In this paper we investigate, in terms of a simple toy model, a possible influence of the (unknown, and therefore ad hoc assumed) vertical dissipation profiles on the vertical structure of the disk and thus on the location of the effective photosphere, and on the observed spectra. For disks with moderate and high mass accretion rates (\dot m>0.01\dot m_C) we find that the photosphere location in the inner, radiation pressure dominated, disk region (where most of the radiation comes from) does not depend on the dissipation profile and therefore emerging disk spectra are insensitive to the choice of the dissipation function. For lower accretion rates the photosphere location depends on the assumed vertical dissipation profile down to the disk inner edge, but the dependence is very weak and thus of minor importance. We conclude that the spectra of optically thick accretion disks around black holes should be calculated with the ray-tracing from the effective photosphere and that, fortunately, the choice of a particular vertical dissipation profile does not substantially influence the calculated spectrum.
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