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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: - PowerPoint PPT Presentation
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Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
The Evolution of Protoplanetary Disks and theThe Evolution of Protoplanetary Disks and the
Diversity of Giant PlanetsDiversity of Giant Planets
The Evolution of Protoplanetary Disks and theThe Evolution of Protoplanetary Disks and the
Diversity of Giant PlanetsDiversity of Giant Planets
Extreme Solar Systems II
September 2011
Ben Bromley Physics & Astronomy, University of Utah
Scott Kenyon Smithsonian Astrophysical Observatory
Extreme Solar Systems II
September 2011
Ben Bromley Physics & Astronomy, University of Utah
Scott Kenyon Smithsonian Astrophysical Observatory
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Diversity of planets
the Solar System: Is it extreme?
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
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)
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Dust-to-planetesimals How do planetesimals grow from micron-sized dust?
Migration How do planetary cores survive (fast, <Myr) migration?
Gas giant formationHow do gas giants grow as gas disks vanish?
Evolution of the gas disk is critical!
Planet formation:difficulties
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Modeling disk evolution
Timing is everything.
HSolid ~ √α
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Simulating planet formation
COAGULATION CODEmergers, fragmentation
growing planetesimalscollisional cascade
FORMATION TIME:
0.1—1 Myr (cores)
1—10 Myr (J,N,SE)
10—100 Myr (Earths)
N-BODY CODEscattering, collisions
photoionization
-viscosity…
gas accretion atmospheres (L,R)migration
PLANETESIMALS:pebbles—plutos
evolve gas, planetesimals, planets in concert
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011log time (yr)
Growth of a planetary system
m /
ME
art
h
sem
imaj
or
axis
(A
U)
150
15
15
3001000
10
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Growth of planetary systems: Jupiters++ (> 1 MJupiter)cu
mu
lati
ve f
ract
ion
log semimajor axis (AU)
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
cum
ula
tive
fra
ctio
n
log semimajor axis (AU)
Growth of planetary systems: Saturns (15 MEarth— 1 MJupiter )
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
cum
ula
tive
fra
ctio
n
log semimajor axis (AU)
Growth of planetary systems: Earths++ (1—15 MEarth)
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
cum
ula
tive
fra
ctio
n
log mass (MJupiter)
Growth of planetary systems: planetary masses
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
cum
ula
tive
fra
ctio
n Growth of planetary systems: Earths+ (1—15 MEarth)Diversity of planets: disk properties
(1—4)
(5—10)
(0—3)
(no gas giants)
(0—3)(2—4)Jupiters
Saturn
s
Super-Earth
s
Earths
log disk viscosity parameter (α)
init
ial
dis
k m
ass
(M)
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
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….
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Simulation summary
photoionization
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Simulation summary
migration
photoionization
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
Diversity of planets
Planetary structure(Radius – Mass, …)
Dynamics(Architecture)
Goal: consistent evolution of full system
Physics and AstronomyUniversity of Utah
Extreme Solar Systems II Fall 2011
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