Quasar Microlensing Variability Studies Favor Shallow Accretion Disk Temperature Profiles
Quasar Microlensing Variability Studies Favor Shallow Accretion Disk Temperature Profiles
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DOI：
10.3847/1538-4357/ab8aed
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发表时间：
2020-06
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影响因子：
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通讯作者：
M. Cornachione;C. Morgan
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文献类型：
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作者：
M. Cornachione;C. Morgan
我们比较了15个引力透镜类星体样本中基于微透镜的连续发射区尺寸测量与基于亮度的薄盘尺寸估计，以约束类星体连续吸积区的温度分布。如果我们采用标准的薄盘模型，我们发现用光度估算的尺寸和用微透镜测量的尺寸之间有显著的差异，log（rL/rμ）= −0.57 ± 0.08 dex。如果类星体连续源是简单的光学厚的吸积盘，具有广义的温度分布T（r）<$r − β，那么微透镜测量和基于亮度的尺寸估计之间的差异可以通过温度分布斜率0.37 < β < 0.56在1σ置信度下解决。在3σ显著性下，这比标准薄圆盘模型（β = 0.75）浅。我们认为交替吸积盘模型，可以产生这样的温度分布和再现经验的连续体大小缩放与黑洞质量，包括磁盘风或磁盘与非黑体大气。
We compare the microlensing-based continuum emission region size measurements in a sample of 15 gravitationally lensed quasars with estimates of luminosity-based thin disk sizes to constrain the temperature profile of the quasar continuum accretion region. If we adopt the standard thin disk model, we find a significant discrepancy between sizes estimated using the luminosity and those measured by microlensing of log(rL/rμ) = −0.57 ± 0.08 dex. If quasar continuum sources are simple, optically thick accretion disks with a generalized temperature profile T ( r ) ∝ r − β , the discrepancy between the microlensing measurements and the luminosity-based size estimates can be resolved by a temperature profile slope 0.37 < β < 0.56 at 1σ confidence. This is shallower than the standard thin disk model (β = 0.75) at 3σ significance. We consider alternate accretion disk models that could produce such a temperature profile and reproduce the empirical continuum size scaling with black hole mass, including disk winds or disks with nonblackbody atmospheres.