DUTREY, Anne; SEMENOV, Dmitry; CHAPILLON, E.; GORTI, Uma; GUILLOTEAU, S.; HERSANT, F.; HOGERHEIJDE, Michiel; HUGHES, Meredith; MEEUS, Gwendolyn; NOMURA, Hideko; PIÉTU, Vincent; QI, Chunhua; WAKELAM, Valentine

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DUTREY, Anne
AMOR 2014

SEMENOV, Dmitry
A.N. Severtsov Institute of Ecology and Evolution

CHAPILLON, E.
AMOR 2014
Institut de RadioAstronomie Millimétrique [IRAM]

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Ce document a été publié dans

Protostars and Planets VI, Henrik Beuther, Ralf S. Klessen, Cornelis P. Dullemond, and Thomas Henning (eds.), University of Arizona Press, Tucson, 914 pp., p.317-338, 2013-07-15, Heidelberg. 2014p. 317-338

Résumé en anglais

Protoplanetary disks composed of dust and gas are ubiquitous around young stars and are commonly recognized as nurseries of planetary systems. Their lifetime, appearance, and structure are determined by an interplay between stellar radiation, gravity, thermal pressure, magnetic field, gas viscosity, turbulence, and rotation. Molecules and dust serve as major heating and cooling agents in disks. Dust grains dominate the disk opacities, reprocess most of the stellar radiation, and shield molecules from ionizing UV/X-ray photons. Disks also dynamically evolve by building up planetary systems which drastically change their gas and dust density structures. Over the past decade significant progress has been achieved in our understanding of disk chemical composition thanks to the upgrade or advent of new millimeter/Infrared facilities (SMA, PdBI, CARMA, Herschel, e-VLA, ALMA). Some major breakthroughs in our comprehension of the disk physics and chemistry have been done since PPV. This review will present and discuss the impact of such improvements on our understanding of the disk physical structure and chemical composition.< Réduire

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Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804