PPT-On the Tilt of Gaseous and Stellar Disks Around the Galacti

Mark Morris UCLA ABSTRACT The welldefined massive disk of young stars orbiting within 05 pc of the Galactic black hole GBH is strongly tilted with respect to the Galactic plane In the context of in situ formation mechanisms this orientation is inherited from that of the gas disk that formed these stars on the order of 6 million years ago The tilt can be understood by positing that clouds fall toward the GBH on nearzero angular momentum orbits and form dispersion rings as they selfintersect after . . atmospheres. a . very. . short. . introduction. Part I. Ewa Niemczura. Astronomical. . Institute. , . UWr. eniem@astro.uni.wroc.pl. Stellar. spectra. Stellar. spectra. One picture is worth 1000 words, but . Gaseous argonManufacture Argon is produced by an air separation unit (ASU) through the liquefactionof atmospheric air and separation of the argon by continuous cryogenicdistillation. The argon is then Giuseppina. . Battaglia. Instituto. de . Astrofisica. de Canarias, Tenerife. Credit. : ESO/. H.H.Heyer. Credit. : ESO/L. . Calçada. Karachentsev. et al. 2014. Individual . Red . Giant Branch . stars. a. nd stellar multiplicity. Insights from recent surveys. Gaspard . Duchêne. (UC Berkeley, Obs. Grenoble). © NASA/JPL/Caltech. Planets in multiple systems?. © . LucasFilm. Ltd.. They must exist!. Phil Armitage. Colorado. Processes in Protoplanetary Disks. Disk structure. Disk evolution. Turbulence. Episodic accretion. Single particle evolution. Ice lines and persistent radial structure. Transient structures in disks. Oxygen is needed for _______________. Oxygen is needed for . cellular respiration.. What is the difference between breathing and gaseous exchange? . Discuss with a peer. 1 and . half minutes. After respiration the oxygen gas . Gaseous Exchange. General factors affecting ‘flow’. F = k * . Δ. P / R. K = constant. Δ. P = delta P, ‘pressure gradient’. R = ‘resistance’ . For exchange of respiratory gases in lungs…. Phil Armitage. Colorado. Motivation. What can we directly observe?. Dust. m. m-mm. Gas – . emission &. kinematics. (CO other. molecules, . H. 2. hard). Limited. direct . time . dependence. Evolution. Pawel. . Artymowicz. U of Toronto. MRI turbulence. Some non-MRI turbulence. Roles and the dangers of turbulence. UCSC Santa Cruz 2010. I borrowed some . figures & slides from. X. Wu (2004). R. Nelson (2008). Insights from recent surveys. Gaspard . Duchêne. (UC Berkeley, Obs. Grenoble). © NASA/JPL/Caltech. Planets in multiple systems?. © . LucasFilm. Ltd.. They must exist!. Planets in multiple systems!. JEFFREY HALL. LOWELL OBSERVATORY, FLAGSTAFF, AZ. Project Timeline. 1988 1992 1996 2000 2004 2008 2012 . Construction/early observing. Rebuild 1. Broad survey. Solar analog survey. Rebuild 2. A/D boundary. Reads and writes are equally fast.. Arrays of these disks are used to provide highly reliable storage.. Increasingly popular as they are fast and do not contain moving parts.. Magnetic Disks.. . What is a magnetic disk and how it works. Two main types: Magnetic and Optical. Random access to memory. The hardware must be controlled by driver software called the “controller” in order to be used. Hard Disks, RAID, and Error Handling. V. . Peskov. CERN. Topics to be covered:. History of detectors of photons and charged particles. Main designs of gaseous detectors. Characteristics and physics of operation. Applications. Modern detectors of photons and charged particles can be classified into four main categories: vacuum, gaseous, liquid and solid–state..