Presidential Young Investigator Award-Active Galactic Nuclei and Supernovae

类星体中发生的物理条件和过程 （类星体）、活动星系、超新星和X射线双星 将从观察的角度进行研究， 再加上理论计算。 大部分研究 将涉及到复杂的形象的发展 处理数据分析技术，以及准确的 吸积盘和电离气体的数值模型。 在 在某些情况下，这些方法可能适用于许多非 天文研究领域。 其中一个主要目标是确定附近的星系 与发光的类星体有任何关系 一般 认为类星体的能量来自于物质的吸积 星系中心的超大质量黑洞。 如果 因此，很可能至少有一些本地星系是“死亡”的。 类星体，因此在它们的原子核中有这样的黑洞。 类似地，类星体现象可能发生在低本征 即使在某些星系中没有发光的类星体， 过去 500个原子核的高质量光谱 在过去的几年里， 将被分析。 在仔细地去除底层 恒星连续谱线和吸收线，微弱发射线 通常可见。 还将进行超新星（SNe）的研究。 一 每个亮SN的一长串光度光谱 将使用北方望远镜进行统计 研究（祖星，与环境的相关性， 等）。 与理论模型预测的比较 应该能揭示出 膨胀气体的机理以及 恒星爆炸 我们将尝试确定 X射线双星的特征，这往往表明 与活动星系核有趣的相似之处。 之一 最重要的问题是， SS 433是一个黑洞或中子星星。 的性质 吸积盘，以及它经历 强迫岁差，也是突出的问题， 解决问题

The physical conditions and processes that occur in quasars (QSOs), active galaxies, supernovae, and X-ray binary stars will be investigated from an observational point of view, coupled with theoretical calculations. Much of the research will involve the development of sophisticated image processing data analysis techniques, as well as accurate numerical models of accretion disks and ionized gases. In some cases the methods may become applicable to many non- astronomical research areas. One of the main goals is to determine whether nearby galaxies are in any way related to luminous QSOs. It is generally believed that QSOs derive their energy from matter accreting onto supermassive black holes in the centers of galaxies. If so, it is likely that at least some local galaxies are "dead" QSOs, and therefore harbor such black holes in their nuclei. Similarly, the QSO phenomenon may occur at a low intrinsic level in some galaxies even if thy were not luminous QSOs in the past. High-quality optical spectra of the nuclei of 500 bright, nearby galaxies, observed during the past few years will be analyzed. After careful removal of the underlying stellar continuum and absorption lines, faint emission lines are usually visible. The study of supernovae (SNe) will also be carried out. A long series of photometric optical spectra of every bright SN accessible to northern telescopes will be used in statistical studies (progenitor stars, correlations with environment, etc.). Comparison with the predictions of theoretical models should shed light on the chemical composition and excitation mechanism of the expanding gas as well as on the nature of the stellar explosion. There will be an attempt to determine the physical characteristics of X-ray binaries, which often show interesting parallels with active galactic nuclei. One of the most important questions is whether the central object in SS 433 is a black hole or a neutron star. The nature of the accretion disk, and the mechanism by which it undergoes forced precession, are also outstanding problems that should be solved.