Origins of giant planets.
"Version: 202112"--Title page verso.Includes bibliographical references.1. The scientific legacy of giant-planet research -- 2. The planet-forming environment -- 2.1. Introduction -- 2.2. Disk evolutionary phases and spectral energy distributions -- 2.3. A simple analytical disk model -- 2.4. Model extensions : adding complexity3. Microscopic to macroscopic : grain growth and pebble formation -- 3.1. Introduction -- 3.2. Gas-dust interaction -- 3.3. Grain growth -- 3.4. Conclusion : how do dust grains evolve?4. From pebbles to planetesimals -- 4.1. Introduction -- 4.2. The planetesimal formation timeline -- 4.3. Mathematical fundamentals of planetesimal-forming instabilities -- 4.4. Numerical models of planetesimal-forming instabilities -- 4.5. Conclusions.Origins of Giant Planets is a comprehensive overview of giant planet formation aimed at new researchers in the field. With the capability of the upcoming James Webb Space Telescope (JWST) to push the mass limit for direct imaging of young planets down to Saturn's scale, observations within the next ten years are likely to bring meaningful constraints to models of giant planet formation.Astronomers and planetary scientists who study giant planets. Graduate students studying exoplanets or planetary science.Also available in print.Mode of access: World Wide Web.System requirements: Adobe Acrobat Reader, EPUB reader, or Kindle reader.Sarah Dodson-Robinson received her PhD in Astronomy & Astrophysics from the University of California at Santa Cruz in 2008, then took a Spitzer Postdoctoral Fellowship at the NASA Exoplanet Science Institute. She is now an Associate Professor of Physics and Astronomy at the University of Delaware.Title from PDF title page (viewed on January 18, 2022).
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