PPT-Probing CO freeze-out and desorption in protoplanetary disks

Author : alida-meadow | Published Date : 2018-02-25

Chunhua Qi HarvardSmithsonian CfA Qi et al 2008 Qi et al in prep Image credit Bill Saxton NRAO Star Formation Stages Sketch of the physical and chemical structure

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Probing CO freeze-out and desorption in protoplanetary disks: Transcript

Chunhua Qi HarvardSmithsonian CfA Qi et al 2008 Qi et al in prep Image credit Bill Saxton NRAO Star Formation Stages Sketch of the physical and chemical structure of a 15 Myr old protoplanetary disk around a Sunlike star. 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. Protoplanetary. Disks. Colette Salyk. National Optical Astronomy Observatory. Credit: JPL-Caltech/T. Pyle (SSC). Credit: NASA. ?. Why studying . protoplanetary. . disks is important for understanding habitability. Lecture by C.P. Dullemond. Institute for Theoretical Astrophysics. Heidelberg University. Image . Credit. : NASA. The Big Questions. After C. Mordasini. > 10 billion galaxies in the Universe. 100 billion stars in each. 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. 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. 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. 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!. Sahil. Singla. . (Carnegie Mellon University). Joint . Work (. Partly) With . ANUPAM GUPTA . and . VISWANATH NAGARAJAN. (2. nd. Feb, 2018). Combinatorial Optimization. Given a . Finite . Universe. Matthew . Marcinkowski. Group Meeting. June 27, . 2016. Adsorption and Desorption. E. ads. E. ads. Non-activated, non-dissociative adsorption. Activated, dissociative process.. Adsorption and Desorption. 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.

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