This book provides a detailed, state-of-the-art overview of key observational and theoretical aspects of the rapidly developing and highly interdisciplinary field of exoplanet science, as viewed through the lenses of eight world-class experts. It equips readers with a broad understanding of the complex processes driving the formation and the physical and dynamical evolution of planetary systems. It juxtaposes theoretical modeling with the host of techniques that are unveiling the exceptional variety of observed properties of close-in and wide-separation extrasolar planets. By effectively linking ingenious interpretative analyses to the main factors shaping planetary populations, the book ultimately provides the most coherent picture to date of the demographics of exoplanetary systems. It is an essential reference for Ph.D. students and early-stage career researchers, while the scope and depth of its source material also provide excellent cues for graduate-level courses.
"Chapter 1:Exoplanet formation by Alessandro Morbidelli, Observatoire de la Cote d'Azur, Nice, France 1.1 Protoplanetary disks structure and evolution 1.1.1 Passive disks 1.1.2 Viscous alpha disks 1.1.3 Origin of viscosity 1.1.4 Disk wind dominated disks 1.2 Dust dynamics 1.2.1 Coagulation 1.2.2 Drift 1.2.3 Trapping in pressure maxima 1.2.4 Streaming instability .3. Accretion of protoplanets 1.3.1 Runaway growth 1.3.2 Oligarchic growth 1.3.3 Pebble accretion 1.4. Type I migration 1.4.1 Lindblad torque 1.4.2 Vortensity and entropy driven corotation torques 1.4.3 Other torques 1.4.4 Migration traps 1.5. Gas accretion and Type II migration 1.5.1 Gas flow in the vicinity of a planet 1.5.2 Hydrostatic contraction of an envelope 1.5.3 Gap opening due to gas repulsion and gas accretion 1.5.4 Migration of giant planets in disks with large or small viscosities 1.6. Resonance trapping during migration 1.6.1 Structure of mean motion resonances 1.6.2 Resonant dynamics during convergent migration 1.6.3 Overstability Chapter 2: Exoplanet dynamics by Sean Raymond, Laboratoire d'Astrophysique de Bordeaux Observatoire de la Cote d'Azur, Nice, France 2.1 Observational constraints and key processes 2.1.1 Constraints from the structure of the Solar System 2.1.2 Meteorites 2.1.3 Observations of protoplanetary and debris disks 2.1.4 Observations of exoplanets 2.1.5 Planet formation models 2.1.6 Planet population synthesis modeling 2.2 Hot super-Earths 2.2.1 Constraints 2.2.2 Formation models 2.2.3 In-situ growth vs migration vs inside-out growth 2.3 Giant exoplanets 2.3.1 Formation 2.3.2 Planet-planet scattering 2.3.3 Migration 2.3.4 Origin models for hot Jupiters 2.4 The standard timeline of Solar System formation 2.4.1 The classical model of terrestrial planet formation 2.4.2 The ""small Mars"" problem 2.4.3 The Nice model 2.5 Alternatives to the classical model 2.5.1 the Grand Tack 2.5.2 Low-mass asteroid belt 2.5.3 Early instability models 2.5.4 Dust drift and planetesimal formation 2.6 Water on Exoplanets 2.6.1 Origin of Earth's water 2.6.2 Water on rocky exoplanets 2.6.3 The diversity of processes and what they predict Chapter 3: Close-in Exoplanets by Andrew W. Howard, California Institute of Technology, USA 3.1 Radial velocity and transit measurement techniques 3.1.1 RV measurements and fitting 3.1.2 Transit measurements and fitting (needed for later lectures) 3.2 Mass, size, and period distributions 3.2.1 Mass distribution of giant planets 3.2.2 Mass distribution of small planets 3.2.3 Size distribution of planets 3.2.4 Orbital period / semi-major axis distributions 3.2.5 Frequency of Habitable Zone planets 3.3 Eccentricity distribution 3.3.1 Origin of eccentricities 3.3.2 Measurement of eccentricities 3.3.3 Giant planet eccentricities 3.3.4 Small planet eccentricities 3.4 Orbital inclination and obliquity 3.4.1 Measurement of inclination and obliquity 3.4.2 Obliquities from Rossiter-McLaughlin and other techniques 3.4.3 Mutual inclinations 3.4.4 Dynamical origins for orbital inclinations 3.5 Planet multiplicity 3.5.1 Intra-system similarity for Kepler multi-planet systems 3.5.2 Singles vs. Multisystems 3.5.3 The Kepler ‘Dichotomy’ 3.6 Ultra-short period planets – distributions and properties 3.6.1 Discovery of USPs - history and initial measurements 3.6.2 Period, size, and mass distributions 3.6.3 Other properties 3.6.4 Physical origins of USPs Chapter 4: Wide-separation Exoplanets by Scott Gaudi, Ohio State University, USA 4.1 Methods of constraining the demographics of planets. 4.1.1 Five main methods of detecting and determining the demographics of exoplanets 4.1.2 Sensitives and selection effects of the five major methods 4.1.3 Methods of calculating unbiased demographics using all five methods 4.1.4 Overlap of the five methods 4.2 The Snow Line and its importance in planet formation theories 4.2.1 What is the snow line? 4.2.2 How is the location of the snow line estimated theoretically? 4.2.3 What are the uncertainties in estimating the location of the snow line? 4.2.4 What are the current and future prospects for estimating the location of the snow line observationally? 4.3 What have direct imaging and microlensing surveys taught us about the demographics of long-period exoplanets? 4.3.1 Lessons learned from first generation Microlensing surveys 4.3.2 Lessons learned from second generation Microlensing surveys 4.3.3 Lessons learned from ground-based direct imaging surveys 4.3.4 Do the results of direct imaging surveys indicate that there are methods of planet formation? 4.4 Results on the demographics of long-period planets from other detection methods and synthesis. 4.4.2 Long baseline RV surveys 4.4.3 Transit surveys: past, present, and future 4.4.4 Synthesizing results from various methods 4.5 The global context of our understanding of planet formation and demographics. 4.5.1 What are the basic results on: 4.5.1.1 The mass function of long period planets 4.5.1.2 The separation distribution of long period planets 4.5.1.3 The population of free-floating planets 4.5.1.4 Comparison with theories of planet formation 4.6 What does the future hold? 4.6.1 TESS 4.6.2 Gaia 4.6.3 WFIRST 4.6.4 PLATO 4.6.5 Reflected Light direct Imaging Mission Chapter 5: Star-Planet interaction by Antonino F. Lanza, INAF - Catania Astrophysical Observatory, Italy 5.1 Star-planet tidal interaction 5.1.1 Equilibrium tides 5.1.2 Dynamic tides 5.1.3 Evolution of stellar angular momentum under the effects of stellar winds 5.2 Tides and the evolution of exoplanets 5.2.1 Evolution of orbital and spin parameters 5.2.2 Tidal energy dissipation inside planets 5.3 Stellar irradiation and planet atmosphere evaporation 5.3.1 Characteristics of stellar high-energy radiation and its relationship with stellar magnetic fields 5.3.2 Simple models of planetary atmosphere evaporation 5.3.3 Impact of irradiation and evaporation on planet evolution 5.4 Star-planet magnetic interactions and their impact on exoplanets 5.4.1 Stellar magnetic field 5.4.2 Planetary magnetic field 5.4.3 Interaction between stellar and planetary magnetic fields 5.4.4 Possible effects of close-by planets on stellar magnetic activity"
Katia Biazzo obtained her PhD in Physics from the University of Catania (Italy) and then worked as a post-doc fellow in several institutes, both abroad (Munich, Strasbourg) and in Italy (Catania, Florence, Naples). Since the end of 2012 she has been a Staff Researcher at INAF - Catania Astrophysical Observatory (currently assigned to the Rome Observatory). Her research interests focus mainly on the search for extrasolar planetary systems (including the characterization of planet hosts) and the study of star formation (including accreting planets and protoplanetary disks). Dr. Biazzo is a member of current and emerging ground (HARPS/HARPS-N, FLAMES, X-Shooter, GIARPS, SHARK, MOONS) and space (JWST, PLATO, ARIEL) based programs. She is the author of about 100 papers in peer-reviewed journals, acts as a reviewer for several journals, and has been co-chair of observing program committees. Valerio Bozza is a Staff Researcher in the Physics Department of Salerno University, Italy.He has worked at CERN with Gabriele Veneziano on string cosmology and cosmological perturbations, and has become an expert on gravitational lensing by black holes, publishing several reviews on the subject. He has developed the fastest publicly available code for modeling planetary microlensing events, which is at the basis of all major existing modeling platforms. Dr. Bozza is a member of the WFIRST Microlensing Science Investigation Team and of several microlensing collaborations searching for extrasolar planets. His real-time modeling platform has become the standard reference in the community for driving follow-up observations. He is responsible for the Astronomical Observatory of Salerno University, performing microlensing observations and validation of transiting extrasolar planets. He is deeply involved in teaching and dissemination, hosting visitors and schools at the Observatory in monthly visits. Luigi Mancini recently became a Research Staff Scientist in the Department of Physics, University of Rome Tor Vergata, Italy, having previously held the same role at the Max Planck Institute for Astronomy, Heidelberg, Germany. He studied Physics and Astrophysics at the University of Salerno, Italy, and then at the University of Zurich, Switzerland. In 2017 he gained Italian National Academic Qualification as a full professor. He is a member of the executive board of the HAT-South Project and works on the detection and characterization of transiting exoplanets. In recent years he has been a collaborator of the JWST Early Release Science working group and a member of other collaborations. He is the author of more than 150 papers in peer-reviewed journals and acts as a reviewer for The Astrophysical Journal and other journals. His h-index is 32. Alessandro Sozzetti gained his degree in Physics from Università degli Studi di Torino, Italy in 1997 and went on to obtain a PhD in Physics from the University of Pittsburgh, USA in 2005. He is a Senior Researcher (Level II) at INAF – Osservatorio Astrofisico di Torino. His research interests focus on the search for, and orbital and physical characterization of, extrasolar planetary systems and brown dwarfs and the characterization of planet hosts (chemical composition, atmospheric and physical parameters). Dr. Sozzetti has leading roles (PI, Co-PI, Chair, Co-I, WP lead) in several ground-based (HARPS-N, GIARPS, ESPRESSO) and space-borne (Gaia, TESS, PLATO, ARIEL) programs aimed at exoplanet detection and characterization. He is coordinator of the EU-funded collaborative project ETAEARTH for the characterization of terrestrial planetary systems with Kepler and HARPS-N and has been co-organizer or co-chair of six major conferences. He is the author of 125 refereed journal papers and has been a contributor to or editor of six collective volumes.
