how do multiple planetary systems shape the dust disk? . - - PowerPoint PPT Presentation

how do multiple planetary systems shape the dust disk?

The HL Tau system

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Giovanni Picogna Tübingen Universität, CPT & Kepler Center 6th May 2015

Exoplanets in Lund 2015 Lund Observatory

. introduction

the hl tau system .

∙ We are now obtaining pristine images of the protoplanetary disk evolution that we can use to constraint planet formation models. ∙ an outstandig example is the HL Tau system, imaged by ALMA in the mm continuum ∙ where axysimmetric ring structures and gaps are visible

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the hl tau system .

∙ We are now obtaining pristine images of the protoplanetary disk evolution that we can use to constraint planet formation models. ∙ an outstandig example is the HL Tau system, imaged by ALMA in the mm continuum ∙ where axysimmetric ring structures and gaps are visible

Figure 1:

HL Tau system. Source: http://www.eso.org/public/news/eso1436/

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the hl tau system .

∙ We are now obtaining pristine images of the protoplanetary disk evolution that we can use to constraint planet formation models. ∙ an outstandig example is the HL Tau system, imaged by ALMA in the mm continuum ∙ where axysimmetric ring structures and gaps are visible

Figure 1:

HL Tau system - continuum 233 GHz image. Source: http://www.eso.org/public/news/eso1436/

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ring structure formation .

There are different physical processes capable of creating rings in a disk: ∙ multi-planetary system ∙ zonal flows

Figure 2: Meru et al., 2014

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ring structure formation .

There are different physical processes capable of creating rings in a disk: ∙ multi-planetary system ∙ zonal flows

Figure 2: Flock et al., 2014

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multi-planetary system scenario .

I focus on the planetary origin of those structure ∙ straightforward explanation ∙ no detailed analysis yet of dust filtration and dynamical evolution in a multi-planetary system

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multi-planetary system scenario .

I focus on the planetary origin of those structure ∙ straightforward explanation ∙ no detailed analysis yet of dust filtration and dynamical evolution in a multi-planetary system

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. numerical method

numerical method .

∙ I have used the FARGO 2D code (Masset et al., 2000) ∙ modified to study the dynamic of a population of small bodies treated as Lagrangian particles (Müller) ∙ integrated with a semi–implicit and fully implicit integrator in cylindrical choordinates as in Zhu et al. (2014) Quantity Value Cells in radial direction 256 Cells in azimuthal direction 512 Inner boundary Open Outer boundary Non–reflecting

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numerical method .

∙ I have used the FARGO 2D code (Masset et al., 2000) ∙ modified to study the dynamic of a population of small bodies treated as Lagrangian particles (Müller) ∙ integrated with a semi–implicit and fully implicit integrator in cylindrical choordinates as in Zhu et al. (2014) Quantity Value Cells in radial direction 256 Cells in azimuthal direction 512 Inner boundary Open Outer boundary Non–reflecting

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numerical method .

∙ I have used the FARGO 2D code (Masset et al., 2000) ∙ modified to study the dynamic of a population of small bodies treated as Lagrangian particles (Müller) ∙ integrated with a semi–implicit and fully implicit integrator in cylindrical choordinates as in Zhu et al. (2014) Quantity Value Cells in radial direction 256 Cells in azimuthal direction 512 Inner boundary Open Outer boundary Non–reflecting

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parameter space .

Physical quantity Value Disk mass (M⊙) 0.135 Disk extent (au) [2.5,100] Aspect ratio 0.05 Viscosity (αSS) 0.004 Surface density profile

• 1

Temperature profile

• 1

EOS Isothermal Dust particles 1 × 106 Dust density (g/cm3) 2.6 Dust size (cm) 0.1,1,10,100 Star mass (M⊙) 0.55 Planet masses (Mth) 1,5,10 Planet semi–major axes (au) 25,50

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limitations .

∙ no self-gravity ∙ no back reaction of the particles on the gas ∙ isothermal EOS ∙ 2D simulations

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limitations .

∙ no self-gravity ∙ no back reaction of the particles on the gas ∙ isothermal EOS ∙ 2D simulations

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limitations .

∙ no self-gravity ∙ no back reaction of the particles on the gas ∙ isothermal EOS ∙ 2D simulations

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limitations .

∙ no self-gravity ∙ no back reaction of the particles on the gas ∙ isothermal EOS ∙ 2D simulations

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. major physical parameters

gap opening criteria .

∙ Thermal criterion Mth = cs3 GΩp = M⋆ (H R )3 Mp M⋆ = q > (H R )3 = 1.25 × 10−4 ∙ Viscous criterion q ≥ 40ν R2

pΩp

= 40αSS (H R )2 = 4 × 10−4

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stopping time .

∙ It quantifies the coupling between the solid and gas components ∙ We adopted the formula by Haghighipour & Boss (2003) that smoothly combines the Epstein and Stokes regimes. τs = τfΩK = ρ•a• ρg [ (1 − f)vth + 3 8fCDvrel ]−1 ΩK FD = − 1 τf ∆vp ∙ For our parameters the dm-size particles have a stopping time ∼ 1

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. results

10 thermal masses .

∙ mm cm dm m –sized particle evolution For videos look at this webpage

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10 thermal masses .

∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital resonance with the inner planet ∙ vortices formation in the inner gap ∙ coorbital regions destabilized by the outer planet ∙ mm-size dust migrate through the gap

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10 thermal masses .

∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital resonance with the inner planet ∙ vortices formation in the inner gap ∙ coorbital regions destabilized by the outer planet ∙ mm-size dust migrate through the gap

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10 thermal masses .

∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital resonance with the inner planet ∙ vortices formation in the inner gap ∙ coorbital regions destabilized by the outer planet ∙ mm-size dust migrate through the gap

Figure 3: cm-sized particles

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10 thermal masses .

∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital resonance with the inner planet ∙ vortices formation in the inner gap ∙ coorbital regions destabilized by the outer planet ∙ mm-size dust migrate through the gap

Figure 3: cm-sized particles

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10 thermal masses .

∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital resonance with the inner planet ∙ vortices formation in the inner gap ∙ coorbital regions destabilized by the outer planet ∙ mm-size dust migrate through the gap

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10 thermal masses .

∙ Final surface density distribution ∙ Final eccentricity distribution

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10 thermal masses .

∙ Final surface density distribution ∙ Final eccentricity distribution

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5 thermal masses .

∙ mm cm dm m –sized particle evolution For videos look at this webpage

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5 thermal masses .

∙ ring fragmentation in 5 high–mass stable points ∙ no long–lived vortex ∙ coorbital regions destabilized by the outer planet ∙ particle exchange between coorbital regions

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5 thermal masses .

∙ ring fragmentation in 5 high–mass stable points ∙ no long–lived vortex ∙ coorbital regions destabilized by the outer planet ∙ particle exchange between coorbital regions

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5 thermal masses .

∙ ring fragmentation in 5 high–mass stable points ∙ no long–lived vortex ∙ coorbital regions destabilized by the outer planet ∙ particle exchange between coorbital regions

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5 thermal masses .

∙ ring fragmentation in 5 high–mass stable points ∙ no long–lived vortex ∙ coorbital regions destabilized by the outer planet ∙ particle exchange between coorbital regions

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5 thermal masses .

∙ Final surface density distribution ∙ Final eccentricity distribution

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5 thermal masses .

∙ Final surface density distribution ∙ Final eccentricity distribution

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1 thermal mass .

∙ mm cm dm m –sized particle evolution For videos look at this webpage

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1 thermal mass .

∙ Ripples in m-sized particles distribution ∙ Particles in coorbital region very close to the planet location ∙ Ring is wider and do not fragment

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1 thermal mass .

∙ Ripples in m-sized particles distribution ∙ Particles in coorbital region very close to the planet location ∙ Ring is wider and do not fragment

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1 thermal mass .

∙ Ripples in m-sized particles distribution ∙ Particles in coorbital region very close to the planet location ∙ Ring is wider and do not fragment

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1 thermal mass .

∙ Final surface density distribution ∙ Final eccentricity distribution

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1 thermal mass .

∙ Final surface density distribution ∙ Final eccentricity distribution

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what’s next? .

∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package) ∙ Extend integration time ∙ Add particle back-reaction ∙ Include disk self–gravity ∙ Different mass planets ∙ Relax isothermal approximation

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what’s next? .

∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package) ∙ Extend integration time ∙ Add particle back-reaction ∙ Include disk self–gravity ∙ Different mass planets ∙ Relax isothermal approximation

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what’s next? .

∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package) ∙ Extend integration time ∙ Add particle back-reaction ∙ Include disk self–gravity ∙ Different mass planets ∙ Relax isothermal approximation

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what’s next? .

∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package) ∙ Extend integration time ∙ Add particle back-reaction ∙ Include disk self–gravity ∙ Different mass planets ∙ Relax isothermal approximation

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what’s next? .

∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package) ∙ Extend integration time ∙ Add particle back-reaction ∙ Include disk self–gravity ∙ Different mass planets ∙ Relax isothermal approximation

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what’s next? .

∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package) ∙ Extend integration time ∙ Add particle back-reaction ∙ Include disk self–gravity ∙ Different mass planets ∙ Relax isothermal approximation

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. conclusions

summary .

∙ particle gaps are very prominent also for small mass planets ∙ co-orbital particles with the inner planet are destabilized ∙ particles in the ring clumps in few stable points ∙ more massive the planets, wider the gap, narrower the ring, more vortices ∙ ripples are observed for particles with high stopping time, orbiting close to small mass planets

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summary .

∙ particle gaps are very prominent also for small mass planets ∙ co-orbital particles with the inner planet are destabilized ∙ particles in the ring clumps in few stable points ∙ more massive the planets, wider the gap, narrower the ring, more vortices ∙ ripples are observed for particles with high stopping time, orbiting close to small mass planets

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summary .

∙ particle gaps are very prominent also for small mass planets ∙ co-orbital particles with the inner planet are destabilized ∙ particles in the ring clumps in few stable points ∙ more massive the planets, wider the gap, narrower the ring, more vortices ∙ ripples are observed for particles with high stopping time, orbiting close to small mass planets

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summary .

∙ particle gaps are very prominent also for small mass planets ∙ co-orbital particles with the inner planet are destabilized ∙ particles in the ring clumps in few stable points ∙ more massive the planets, wider the gap, narrower the ring, more vortices ∙ ripples are observed for particles with high stopping time, orbiting close to small mass planets

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summary .

∙ particle gaps are very prominent also for small mass planets ∙ co-orbital particles with the inner planet are destabilized ∙ particles in the ring clumps in few stable points ∙ more massive the planets, wider the gap, narrower the ring, more vortices ∙ ripples are observed for particles with high stopping time, orbiting close to small mass planets

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summary .

∙ the simulations with 1 thermal mass planets present wider rings and narrow gaps, creating a similar dust distribution as observed by the ALMA telescope ∙ if this is the case the gas emission from the same system is expected to be much more smooth

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summary .

∙ the simulations with 1 thermal mass planets present wider rings and narrow gaps, creating a similar dust distribution as observed by the ALMA telescope ∙ if this is the case the gas emission from the same system is expected to be much more smooth

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Questions?

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