标题： 受辐射压支持的星暴盘和活动星系核供气 显示英文标题

标题： Radiation Pressure Supported Starburst Disks and AGN Fueling

摘要： 我们研究了在辐射压力对尘埃颗粒的垂直支持起主导作用的情况下，边缘托尔内稳定性恒星爆发盘的结构。当盘面对自身的红外辐射是光学厚的时候，这尤其适用，正如在ULIRG（超亮红外星系）中心区域的情况一样。 由于盘面以爱丁顿极限发光，恒星形成施密特定律在光学厚极限下发生变化，单位面积的恒星形成率与气体表面密度Sigma_g和平均消光系数kappa成反比关系。 我们显示，光学厚恒星爆发盘具有一个特征通量和尘埃有效温度，分别为F ~ 10^{13}L_sun/kpc^2 和T_eff ~ 90K。 我们将预测结果与观测数据进行比较，并发现良好的一致性。 我们将模型从数百帕斯卡尺度扩展到亚帕斯卡尺度，并解决AGN供能问题。 我们假设角动量传输通过全局扭矩而不是局部粘度来实现。 我们考虑到由于恒星形成导致的气流径向耗尽，并发现了两类盘面模型之间强烈的二分法：(1) 大规模爆发消耗所有气体且中央AGN供能较少的解；(2) 外部大规模爆发伴随1-10 pc尺度上更紧凑的爆发以及明亮中央AGN的模型。 后一类模型的亮度在许多情况下由AGN主导。 我们表明，在pc尺度上的恒星爆发盘的垂直厚度可以接近h ~ r，或许解释了一些II型AGN中的核区遮蔽现象。 我们还提出银河系中心的年轻恒星盘可能是此类紧凑核区恒星爆发的遗迹。 显示英文摘要

摘要： We consider the structure of marginally Toomre-stable starburst disks under the assumption that radiation pressure on dust grains provides the dominant vertical support against gravity. This is particularly appropriate when the disk is optically thick to its own IR radiation, as in the central regions of ULIRGs. Because the disk radiates at its Eddington limit, the Schmidt-law for star formation changes in the optically-thick limit, with the star formation rate per unit area scaling as Sigma_g/kappa, where Sigma_g is the gas surface density and kappa is the mean opacity. We show that optically thick starburst disks have a characteristic flux and dust effective temperature of F ~ 10^{13} L_sun/kpc^2 and T_eff ~ 90K, respectively. We compare our predictions with observations and find good agreement. We extend our model from many-hundred parsec scales to sub-parsec scales and address the problem of fueling AGN. We assume that angular momentum transport proceeds via global torques rather than a local viscosity. We account for the radial depletion of gas due to star formation and find a strong bifurcation between two classes of disk models: (1) solutions with a starburst on large scales that consumes all of the gas with little fueling of a central AGN and (2) models with an outer large-scale starburst accompanied by a more compact starburst on 1-10 pc scales and a bright central AGN. The luminosity of the latter models is in many cases dominated by the AGN. We show that the vertical thickness of the starburst disk on pc scales can approach h ~ r, perhaps accounting for the nuclear obscuration in some Type 2 AGN. We also argue that the disk of young stars in the Galactic Center may be the remnant of such a compact nuclear starburst.