Formation of Giant Planets

Giant planets are tens to thousands of times as massive as the Earth, and many times as large. Most of their volumes are occupied by hydrogen and helium, the primary constituents of the protostellar disks from which they formed. Significantly, the solar system giants are also highly enriched in heavier elements relative to the Sun, indicating that solid material participated in their assembly. Giant planets account for most of the mass of our planetary system and of those extrasolar planetary systems in which they are present. Therefore, giant planets are primary actors in determining the orbital architectures of planetary systems and, possibly, in affecting the composition of terrestrial planets. This Chapter describes the principal route that, according to current knowledge, can lead to the formation of giant planets, the core nucleated accretion model, and an alternative route, the disk instability model, which may lead to the formation of planetary-mass objects on wide orbits.Comment: Invited review, accepted for publication in the "Handbook of Exoplanets", eds. H.J. Deeg and J.A. Belmonte, Springer (2018). 28 pages, 8 figure

An Annotated Bibliography for Post-solution Analysis in Mixed Integer Programming and Combinatorial Optimization

Abstract This annotated bibliography focuses on what has been published since the 1977 Geoffrion-Nauss survey, and it is in BibTEX format, so it can be searched on the World Wide Web. In addition to postoptimal sensitivity analysis, this survey includes debugging a run, such as when the integer program is unbounded, anomalous or infeasible