Transient X-ray Binaries In Centaurus A. Gregory R. Sivakoff ( UVa ) Chandra Cen A- Very Large Project Team. A Galaxy’s Cookbook A Population of X-Ray Binaries Start With A Galaxy’s Stellar IMF # NSs/BHs Stir In Stellar Dynamics # Binaries FormBy audra
THE MOON SATELLITE. BY J.JAYASREE M.TECH-COS. Moon:. The Moon is the Earth's only natural satellite, circling in a slightly elliptical orbit at 2,300 miles per hour (3,683 km/hr).By mimir
Relativistic Emission Lines of Accreting Black Holes. Andreas Müller 21. Mai 2003. Quasare und früher Kosmos Forschungsseminar LSW. Overview. Motivation AGN paradigm AGN X-ray spectra X-ray fluorescence Coronal irradiation Rotating black holes and Kerr ray tracingBy tulia
Basic Theory. Matter was created Stars were an error. Protoplanet Hypothesis. 5 billion years ago a clod of dust and gas 10 billion km in diameter rotated. As time passed the cloud shrank under its own gravity, or collapsed from an explosion.By kuame-chan
Relativistic Emission Lines of Accreting Black Holes. Andreas Müller 21. Mai 2003. Quasare und früher Kosmos Forschungsseminar LSW. Overview. Motivation AGN paradigm AGN X-ray spectra X-ray fluorescence Coronal irradiation Rotating black holes and Kerr ray tracingBy kjensen
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ACCRETION. WINDS. Inflow…. Outflow…. Martin Ward, University of Durham. X-ray/UV Outflows and the Coronal Emission Lines. Outflows are ubiquitous. b. Winds in general. Analogy with jets, they can tell us about bulk energy transport, and provide an imprint of past activity
Accretion Disks. Prof. Hannah Jang-Condell. Accretion Disks. Neutron Star (artist’s conception). Galaxy: M81. Protoplanetary Disk: AB Aurigae. (Giovanni Benintende ). ( Fukagawa , et al. 2004). (M . Masetti , NASA). Why are disks so common?. Why are disks so common?.
Accretion #3. When is the thin disk model valid? Reynolds number, viscosity Time scales in disk BH spectra Using X-ray spectra to determine BH mass and spin Using emission lines to determine BH spin. X-Ray Spectrum. Thermal emission from disk - multicolor blackbody
Lecture 4. AST3020. Accretion disks. Flaring shape jets. Outflows disappear before the disks do. High!. (on the other hand, in debris disks which don’t have a lot of gas and much less dust as well, both the opacity of dust and the
Terrane accretion. GEOS 304 - 2009. Terrane. Out of place large piece of lithosphere Bounded by major plate margin faults Ophiolites present if the motin was not transform Geology different from adjacent lithosphere Identifiable source. Present day config (Miller et al., 2006).
Theory of quasi-spherical accretion in X–ray pulsars. Shakura et al. Reporter: Zhang Zhen 11.11.28. A theoretical model for quasi-spherical subsonic accretion onto slowly rotating magnetized neutron stars Quasi-spherical shell Convective motions. Outlines. Introduction
Accretion of Planets. Star & Planet Formation Minicourse, U of T Astronomy Dept. Lecture 5 - Ed Thommes. Bill Hartmann. Overview. Start with planetesimals : km-size bodies, interactions are gravitational