Particle Trapping in Protoplanetary Disks: Models vs. Observations
Abstract
With modern astronomical observatories, such as ALMA<IndexTerm ID="ITerm1"> <Secondary>ALMA (Atacama Large Millimeter Array)</Secondary> , we are now able to constrain the physical processes that govern planet formation<IndexTerm ID="ITerm2"> by confronting model predictions with observations. Of particular interest is the growth and evolution of dust grains<IndexTerm ID="ITerm3"> into larger solids, a crucial first step in the formation of planetesimals that shapes the diversity of exoplanetary systems. In traditional disk models, with smooth radial gradients<IndexTerm ID="ITerm4"> <Secondary>radial</Secondary> , dust growth<IndexTerm ID="ITerm5"> <Secondary>dust-</Secondary> inevitably leads to the fast inward migration of pebbles, a challenge to understanding both planet formation and disk observations. However, recent high resolution observations at different wavelengths show that disks are not smooth, but show diverse structures, including rings, asymmetries, dips of emission, and spiral arms<IndexTerm ID="ITerm6"> . In this chapter, we summarize how models of evolving gas and dust disks<IndexTerm ID="ITerm7"> <Secondary>dust-</Secondary> can explain these observed structures. We explore several phenomena that can create particle traps in gas disks<IndexTerm ID="ITerm8"> <Secondary>gas-</Secondary> , such as magneto-rotational instabilities and embedded planets. We place these models in the context of planetesimal formation theory broadly, and discuss open questions and future opportunities for both theoretical and observational work.
- Publication:
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Formation, Evolution, and Dynamics of Young Solar Systems
- Pub Date:
- 2017
- DOI:
- 10.1007/978-3-319-60609-5_4
- Bibcode:
- 2017ASSL..445...91P
- Keywords:
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- Physics