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The Evolution of Protoplanetary Disks and the Diversity of Giant Planets

The Evolution of Protoplanetary Disks and the Diversity of Giant Planets. Extreme Solar Systems II September 2011 Ben Bromley Physics & Astronomy, University of Utah Scott Kenyon Smithsonian Astrophysical Observatory. Diversity of planets. the Solar System:

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The Evolution of Protoplanetary Disks and the Diversity of Giant Planets

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  1. The Evolution of Protoplanetary Disks and the Diversity of Giant Planets Extreme Solar Systems II September 2011 Ben Bromley Physics & Astronomy, University of Utah Scott Kenyon Smithsonian Astrophysical Observatory

  2. Diversity of planets the Solar System: Is it extreme?

  3. Planet formationtheory and practice • Young stars: gas/dust disk • Coagulation and dynamics; collisional accretion (many, small  few, large) • Debris disks are signpostsof planet formation • Massive cores accrete gas (entrained debris helps, tGas ~ Myr)

  4. Planet formation: difficulties • Dust-to-planetesimals How do planetesimals grow from micron-sized dust? • Migration How do planetary cores survive (fast, <Myr) migration? • Gas giant formation How do gas giants grow as gas disks vanish? Evolution of the gas disk is critical!

  5. Modeling disk evolution • Initial conditions (Mdisk = 0.003—0.1 MStar; solid:gas ~ 0.01; S~ 1/a0.6—1.5) • Input physics (alpha disk: a = 10-5—0.01; tDisk ~ 1/a~ 1—10 Myr) • evolving the disk (solve diffusion equation)  HSolid ~ √α  Timing is everything.

  6. Simulating planet formation PLANETESIMALS: pebbles—plutos FORMATION TIME: 0.1—1 Myr (cores) 1—10 Myr (J,N,SE) 10—100 Myr (Earths) a-viscosity… Coagulation code mergers, fragmentation photoionization growing planetesimals collisional cascade N-BODY CODEscattering, collisions gas accretion atmospheres (L,R) migration evolve gas, planetesimals, planets in concert

  7. Growth of a planetary system 150 15 15 300 1000 10 m / MEarth semimajor axis (AU) log time (yr)

  8. Growth of planetary systems: Jupiters++ (> 1 MJupiter) cumulative fraction log semimajor axis (AU)

  9. Growth of planetary systems: Saturns (15 MEarth— 1 MJupiter ) cumulative fraction log semimajor axis (AU)

  10. Growth of planetary systems: Earths++ (1—15 MEarth) cumulative fraction log semimajor axis (AU)

  11. Growth of planetary systems: planetary masses cumulative fraction log mass (MJupiter)

  12. Growth of planetary systems: Earths+ (1—15 MEarth) Diversity of planets: disk properties Jupiters (0—3) (2—4) (1—4) Saturns Super-Earths initial disk mass (M) (0—3) cumulative fraction (5—10) Earths (no gas giants) log disk viscosity parameter (α)

  13. Results • Diverse systems of gas giants in alpha-disk model • Predictions: Multiplanet systems, ~MEarth—10’s of Mjupiter High mass, low viscosity disks: Jupiters Low mass, high viscosity disks: Neptunes, super-Earths • Next step: Include photoionization, migration….

  14. Simulation summary photoionization

  15. Simulation summary migration photoionization

  16. Diversity of planets Dynamics (Architecture) Planetary structure (Radius – Mass, …) Goal: consistent evolution of full system

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