PPT-The Magnetic Origin of Black Hole Accretion Disk Winds

Author : lois-ondreau | Published Date : 2019-12-10

The Magnetic Origin of Black Hole Accretion Disk Winds Chris Shrader NASA Goddard Space Flight Center Collaborators D Kazanas GSFC K Fukumura JMU F Tombesi UMD

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The Magnetic Origin of Black Hole Accretion Disk Winds: Transcript

The Magnetic Origin of Black Hole Accretion Disk Winds Chris Shrader NASA Goddard Space Flight Center Collaborators D Kazanas GSFC K Fukumura JMU F Tombesi UMD Ehud Behar . What is Whole Disk Encr yp tion Whole Disk Encr yp tion versus File Encr yp tion Ramesh Narayan. Jets are Widespread. Relativistic Jets . occur widely in . accreting black holes (BHs): AGN, XRBs, GRBs. A . common . robust . mechanism . must be producing all these . Jets. Best Bet. Gamma ray bursts (GRB) are an especially exciting outflow phenomena that are capable of outputting as much energy as our sun will. Christopher C. . Lindner. 1. Abstract. Relativistic Jets are streams of plasma moving throughout the universe at speeds up to 99% the speed of light. They produce high-energy X-ray, radio, and visible radiation that are observable from great distances across the universe. young stars . with . LSST. Gregory J. Herczeg. KIAA. Star Formation: . ISM/Molecular Clouds . Pre-main sequence stellar evolution. (low-mass case). HD141569, . Clampin. et al.. Classical T . Tauri. Stars. Christopher C. Lindner, . Milos. . Milosavljevic. , Sean Couch, . Pawan. Kumar. . The University of Texas at Austin. Results. We have conducted hydrodynamic simulations of the viscous post-core-collapse accretion of a rapidly rotating 14 solar mass Wolf-. 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. . We . performed nine simulations to test the sensitivity of our results to resolution, viscous stress-to-pressure ratio (α), the initial rotation parameter (. ξ. l. ), convective energy transport efficiency (. and Outburst Mechanisms. Zhaohuan. Zhu. Hubble Fellow, Princeton University. Collaborators: Lee Hartmann (. Umich. ), Charles . Gammie. (UIUC), . . Nuria. . Calvet. (. Umich. Ted Jacobson. University of Maryland. Gravity and Black Holes, Cambridge, July 4, 2017 . Wheeler to . Bekenstein. (1971):. “If I drop a teacup into a black hole, . I conceal from all the world the. 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). The Magnetic Origin of Black Hole Accretion Disk Winds Chris Shrader* (NASA Goddard Space Flight Center ) Collaborators: D. Kazanas (GSFC), K. Fukumura (JMU), F. Tombesi (UMD), Ehud Behar ( Screw And Surface. Counterbore. Countersink. Threaded hole. Clearance Hole. Category 5? typical gusts over open flat land of more than 280km/h. These winds correspond to the highest category on the Beaufort Scale. Extremely dangerous with widespread destruction. One of the Prof Chris Done. University . of Durham & ISAS/JAXA. AGN feedback. Magorrian-Gebhardt. relation gives BH mass!! Big black holes live in host galaxies with big bulges! Either measured by bulge luminosity or bulge mass (stellar velocity dispersion) or .

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