giant planets around young m-dwarfs › ~dmawet › meetings › mdwarfs.pdfjupiter. giant planet...
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Giant planets around young M-dwarfs
Henry Ngo (Caltech)
D Mawet, B Bowler, J Wang, O Absil, M Bottom, E Choquet, C Gomez, E Huby, L Hillenbrand,
R Jensen-Clem, T Meshkat, M Reggiani, E Serabyn
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Semimajor axis (AU)
Plan
et M
ass
(MJu
p)
Transit Radial Velocity Microlensing
Direct Imaging
Jupiter
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Giant Planet Formation
1) Core formation
2) Hydrostatic growth
3) Runaway accretion
4) Planet contracts
Source of gas is removed
Core reaches ~10 Earth masses
Core mass ≈ envelope mass
(and emits energy we can detect)
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Challenges • Gather enough solids for critical mass • Reach critical mass before gas dissipates
1) Core formation
2) Hydrostatic growth
3) Runaway accretion
4) Planet contracts
Source of gas is removed
Core reaches ~10 Earth masses
Core mass ≈ envelope mass
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Batygin et al. (2016)
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Enough solids? Minimum Mass Extrasolar Nebula Chiang & Laughlin (2013) Efficient enough? Compact multi-planet systems Boley et al. (2016) Batygin et al. (2016)
in situ formation
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formation then migration
Enough solids? Increase in solids at ice line Lin et al. (1996) Efficient enough? “Pebble accretion” Lambrechts & Johansen (2012)
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Predictions • in situ formation: additional smaller planets, P < 100 d
• ice line formation & migration: planet reservoir?
iceline(severalAU)
Young planets Old planets
(observed today)
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Predictions • in situ formation: additional smaller planets, P < 100 d
• ice line formation & migration: planet reservoir?
iceline(severalAU)
Young planets Old planets
(observed today) Q: Does this ice-line planet reservoir exist?
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Finding young planets at the ice lines
• Target young moving group members
Bowler (2016): Recent efforts to find low-mass members creates large number of potential direct imaging targets
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Knowing age is important
Bowler (2016)
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Maximize detection ability
Bowler (2016)
Young stars Nearby stars Smaller stars
= better contrast
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Detection Probability Sample of 200 late K / M-dwarf (<d> = 40 pc)
L’ vortex on Keck/NIRC2 (IWA = 80 mas)Expected yield (microlensing): 10 planets
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Sample star in beta Pic43 pc, 20 Myr, rmag ~9.5
Science image, flattened ADI+PCA processed
(VIP; Gomez Gonzalez et al. 2016)
~ 3”
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Sample star in beta Pic43 pc, 20 Myr, rmag ~9.5
5x10-4 contrast @ 0.5”3 MJ @ 22 AU
2x10-3 contrast @ 0.3”6 MJ @ 13 AU
Expect improved contrast down to ~ 0.1” with RDI correction
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Progress (since Oct 2015) Schedule
Planned:
4 semesters
Completed: 2 semesters
Next semester (2016B) already
allocated.
Apply for final semester (2017A)
next month
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Summary • Two hot Jupiter formation models – in situ: predicts additional small planets with
periods < 100 days – migration: predicts reservoir of young planets
near ice line • Survey of ~200 M-dwarfs in L-band on
Keck/NIRC2 with vortex to confirm or refute ice line planet reservoir
• Reggiani/Absil: Southern survey on VLT