Institute for. Advanced Study. Multi-planetary systems. Hanno of Toronto, Scarborough, March 2013
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1 Institute for Advanced Study Multi-planetary systems Hanno of Toronto, Scarborough, March 2013
2 Projects that I will not talk about today Symplectic integrators Viscous overstability Parallel tree codes Stability of exo-moons Open Exoplanet Catalogue Simulations of dense rings
3 All discovered extra-solar planets 869 confirmed extrasolar planets Super-Jupiters (Hot) Jupiters Neptunes Super-Earths Earth-size planets Open Exoplanet Catalogue (Rein 2012b)
4 All multi-planetary systems 869 confirmed extrasolar planets Super-Jupiters (Hot) Jupiters Neptunes Super-Earths Earth-size planets Open Exoplanet Catalogue (Rein 2012b)
5 Take home message I There are a lot of planets.
6 Exoplanets Available for free on the AppStore. Exoplanet App by Hanno Rein Available on the Apple AppStore
7 Take home message II The variety of planets and planetary systems is enormous.
8 Recipe: 1. Planet migration 2. Resonances
9 1. Planet migration
10 Planet formation Image credit: NASA/JPL-Caltech
11 Smooth migration 2D hydro code Prometheus (Rein 2010)
12 Stochastic migration Animation from Nelson & Papaloizou 2004 Random forces measured by Laughlin et al. 2004, Nelson 2005, Oischi et al. 2007
13 Take home message III planet + disc = migration
14 2. Resonances
15 2:1 Mean Motion Resonance Star Planet 1 Planet 2
16 Asteroids in resonance with Jupiter Scott Manley
17 Saturn s rings are sculpted by resonances
18 The system Gliese 876 Massive planets. Locked in a resonance. Observed with high accuracy. Open Exoplanet Catalogue (Rein 2012b)
19 Take home message IV Resonances are special dynamical configurations.
20 Formation of GJ 876: Resonance capture Migration can explain this special resonant configuration Both the period ratio and the eccentricities are reproduced Lee & Peale 2002, Rein et al 2012
21 Take home message V 2 planets + migration = resonance
22 The case of Kepler-36
23 Kepler-36 c as seen from Kepler-36 b Would appear 2.5 times the size of the Moon Very close orbits, near a 7:6 resonance Very different densities Carter et al (2012), Frank Melchior, Eric Agol
24 Snow line Rocky material Icy material Image credit: NASA/JPL-Caltech
25 Convergent migration in Kepler-36 icy planet rocky planet Successful formation scenario for Kepler-36 Getting planets of different origin (composition) close together Forming stable high order resonances Capture probability greatly enhanced by adding a small amount of stochastic migration Paardekooper, Rein & Kley (in prep)
26 Take home message VI We find planets where they didn t form. This is a result of migration.
27 The formation of HD45364
28 HD Observations Correia et al radial velocity [m/s] JD [days] Correia et al 2009, Visual Exoplanet Catalogue
29 Formation scenario for HD45364 semi major axis period ratio eccentricity eccentricity period ratio semi major axis H. Rein et al.: The dynamical origin of HD time Fig. 2. The semi-major axes (top), period ratio P2 /P1 (middle), and eccentricities (bottom) of the two planets plotted as a function of time in dimensionless units for run F5 with a disc aspect ratio of h = In time 1500 Fig. 4. The semi-major axes (top), period ratio P2 /P1 centricities (bottom) of the two planets plotted as a fu Rein, Kley 2010 dimensionless units for Papaloizou run F4 with a&disc aspect ratio
30 Lessons learned from HD45364 Massive disc (5 times MMSN) Short, rapid migration Passage of 2:1 resonance Capture into 3:2 resonance Large scale-height (0.07) Slow migration once in resonance Resonance is stable Rein, Papaloizou & Kley 2010
31 Take home message VII Migration scenarios provide us with valuable information about the environment of planet formation.
32 Testable predictions! 40 Observations Correia et al Simulation F radial velocity [m/s] JD [days] Our formation model predicts a specific set of orbital parameters Consistent with current observations Testable with just a few well-timed radial velocity data points. Rein, Papaloizou & Kley 2010
33 HD The impossible system?
34 HD Two massive planets 1.8 MJup and 0.9 MJup Period ratio close to 4:3 Another similar system, to be announced soon. Rein, Payne, Veras & Ford (2012)
35 Stability of HD :3 "< cat output*.txt pgt_pm3d 3 4 5" u 1:2:($3>0?$3:0.1-$3) unstable 0.6 2:1 5:2 eccentricity e : stable semi-major axis a 2 [AU] Rein, Payne, Veras & Ford (2012)
36 Take home message VIII We don't understand everything*. *just yet
37 Saturn s Rings
38 Saturn is a smaller version of the Solar System
39 Stochastic Migration REBOUND code, Rein & Papaloizou 2010, Crida et al 2010
40 Summary The formation of multi-planetary systems Many planets are in systems where multiple planets orbit the same star. By studying the current dynamical configuration we can learn a lot about the physical environment at the time when the planets formed. Gliese 876 Kepler-36 HD45364 HD Best example for the effects of dissipative planet migration. Very different composition, brought onto close orbits by migration. Had to form in a massive disc. We have no clue (yet). The big picture Understanding the formation of multi-planetary systems is essential if we want to know if the Solar System is special, if life is special.
41 Exoplanet Visualization Contest openexoplanetcatalogue.com/contest/
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