PPT-Turbulence in accretion disks

Pawel Artymowicz U of Toronto MRI turbulence Some nonMRI turbulence Roles and the dangers of turbulence UCSC Santa Cruz 2010 I borrowed some figures amp slides from X Wu 2004 R Nelson 2008. Alecian Abstract In this chapter I 64257rst present the premain sequence stars around which accretion disks are observed and summarise the main observed characteristics of the classical T Tauri and Herbig AeBe stars I then review the theoretical and 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. 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. Topic:. Turbulence. Lecture by: C.P. Dullemond. The idea behind the α-formula. Viscosity is length times velocity:. Maximum height of an eddy: . Maximum velicity of an eddy: . The idea behind the α-formula. AS 4024 InclinationsRadial velocities give minimum masses•need inclinations– orbits–eclipsing binaries–apsidal motion 333 AS 4024 Binary Stars and Accretion Disks Astrometric Orbit http://turb.seas.ucla.edu/~jkim/sciam/turbulence.html Turbulence ? Why do the skin of sharks have groves ? Related Links But what exactly is turbulence? A few everyday examples may be illuminati 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. 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. 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. 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. Bas van de . Wiel. , . Ivo. van . Hooijdonk. & Judith . Donda. in collaboration with:. Fred . Bosveld. , Peter Baas, . Arnold . Moene. , Harm . Jonker. , . Jielun. Sun, Herman Clercx, . e.a. .. 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. 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 ( 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 (