Formation and Structure of High-z quasars

根据结构形成的标准场景，质量约为10^7太阳质量的旋转暗物质盘预计会在高红移（z-几百）形成。这些圆盘是否会演化成类星体取决于后来的圆盘演化。为了讨论黏度和自重力作用下的圆盘演化，我们寻求了自相似解，并找到了自相似解。我们还研究了背景辐射导致的康普顿阻力如何影响粘性盘的演化，发现阻力和粘性实际上是相互加强的，从而促进了磁盘的快速坍缩。现在，由如此巨大的自引力盘形成原类星体黑洞的可能性已经成为现实。我们还发现了一种新的方法来观测高红移类星体的中心结构。这就是所谓的引力微透镜；也就是说，当恒星经过类星体的图像时，一小部分的辐射会被选择性地放大。事实上，我们已经将这种方法应用于爱因斯坦交叉（Q02237），发现一个假定的黑洞周围的圆盘的发射特性将在空间尺度上分解到几个史瓦西半径。我们现在等待进行这种观察。

According to the standard scenario for structural formation, rotating dark-matter disks with mass of about 10^7 solar masses are expected to form at high red-shifts (z-several hundreds). Whether such disks would evolve to quasars depend on later disk evolution. To discuss the disk evolution under the influence of viscosity and selt-gravity, we have seeked for self-similar solutions and could find them. We have also examined how Compton drag due to background radiation affect viscous disk evolution, finding that drag and viscosity actually reinforce each other, thereby rapid disk collapse being promoted. Now the possibility to form a proto-quasar black hole by such a massive self-gravitating disk has become realistic.We have also found a novel method to observationally resolve the central structure of high redshift quasars. This is to use the so-called gravitational microlensing ; namely, when stars pass by the image of a quasar, radiation from a tiny portion will selectively be amplified. We have in fact apply this method to Einstein Cross (Q02237), finding that emission properties of the disk around a putative black hole will be resolved on spatial scales down to several Schwarzschild radii. We now await until such observations will be performed.