论文标题
五角体变异性研究有利于浅盘温度曲线
Quasar Microlensing Variability Studies Favor Shallow Accretion Disk Temperature Profiles
论文作者
论文摘要
我们比较了15个重力透镜类星体样品中基于微透镜的连续发射区域大小的测量值，并估计了基于亮度的薄磁盘大小，以限制类星体连续体积聚区域的温度曲线。如果我们采用标准的薄磁盘模型，我们会发现使用光度估计的尺寸与通过微透明$ \ log（r_ {l}/r_μ）= -0.57 \ pm0.08 \，\ text {dex} $测量的尺寸显着差异。如果Quasar Continuum源很简单，具有通用温度曲线$ t（r）\ Propto r^{ - β} $的光学厚度积分磁盘，则可以通过温度型号$ 0.37 <β<β<β<β<0.56 $ at $ 1 \ 1 prefiners $ 0.37 <0.56 $ profforts $ profections r^{ - β} $ r^{ - β} $。这比标准的薄磁盘模型（$β= 0.75 $）在$ 3 \，σ$显着性时浅。我们考虑可以产生这种温度曲线的替代积聚磁盘模型，并以黑洞质量（包括磁盘风或具有非黑色体气氛的磁盘）重现经验连续体尺寸。
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 $\log(r_{L}/r_μ)=-0.57\pm0.08\,\text{dex}$. If quasar continuum sources are simple, optically thick accretion disks with a generalized temperature profile $T(r) \propto r^{-β}$, 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 $1\,σ$ confidence. This is shallower than the standard thin disk model ($β=0.75$) at $3\,σ$ 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 non-blackbody atmospheres.
