Recent advances in understanding planet formation
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- Roderick Lester
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1 Credit: ALMA (ESO/NAOJ/NRAO) Recent advances in understanding planet formation Misato Fukagawa Chile observatory (Mitaka), NAOJ
2 Contents of this talk 1. Introduction: Exoplanets, what we want to know from observations of protoplanetary disks 2. Recent observations Dust mass and its evolution available time/material for planet formation Grain growth necessary step toward planet formation Azimuthal asymmetry sign of ongoing formation Multiple, symmetric gaps in HL Tau 3. What will come, what we want to have near future Chemical study is not included in this review.
3 Planets are common
4 Diversity
5 2 Jupiter-mass at 13 AU in direct imaging We ve started to detect planets like in our Solar-system 0.99 Jupiter-mass at 4.8 AU around a star with ~6000 K NASA Ames/JPL-CalTech/R. Hurt
6 Questions How did the solar system (in particular, our Earth) form? How do planets form in the Milky way? What is the key to form Solar-system-like planetary systems?
7 1. Formation 2. Migration Interaction with a disk Interaction with other planets Diversity? Credit: NAOJ
8 Giant planet formation Standard senario: Core accretion Takes ~10 million years (~1 Myr at the fastest) Dust (micron) -> planetesimals (~km) Gas accretion Credit: Rikanenpyo
9 Disks provide initial condition of formation and control early orbital evolution of planets Surface density distribution (disk mass) Planet mass and location Chemical evolution of disk material Planet composition Disk gas lifetime, dissipation mechanisms Orbital evolution (migration) of planets What we want to know: Physical and chemical structure (r, z), T(r, z), X(r, z) X-ray, UV, optical accretion radial drift mixing
10 Key things for protoplanetary disk 1. High angular resolution observations Distance to the nearest star-forming regions ~ 140 pc Want to spatially resolve ~5 AU (Jupiter s orbit) ~30 milliarcsec is required. (ALMA, adaptive optics in optical on 8m class telescopes) 2. Longer wavelengths Mid-plane (where planets form) has very high density. Most region is optically thick if < submillimeter. Large grains are bright at longer wavelengths.
11 Protoplanetary disks frequently observed 0.1 Myr Age: 1 10 million years Optically thick, gaseous 1. Planet will form Initial condition 2. Formation has just completed Dynamical interaction between disk and planets Young planets 1 Myr 10 Myr 100 Myr NAOJ
12 Dust mass and its evolution in protoplanetary disks amount and lifetime of ingredients of planets
13 Disk (mm-dust) mass from dust continuum M disk ~ F d 2 B (T d ) M disk M star 1 solar mass Careful analysis of SMA 1.3 mm 1% of the star Dust mass is roughly proportional to the stellar mass. There is a significant scatter. Jupiter Andrews et al. (2013)
14 Disk (mm-dust) mass evolution ALMA, 880 micron continuum U Sco: Age = 5 11 Myr Sensitivity: an order of magnitude better than the previous survey. Minimum detected mass = 0.3 Earth-mass No significant difference, or marginal evidence of lower mass compared to he younger region at ~2 Myr. -- need more data. Carpenter et al. (2014) 14
15 Grain growth fundamental step toward planets
16 Grain growth Dust continuum Brightness distribution is frequency dependent. Perez et al. (2012)
17 Β<1 Grain growth β is not constant in radial direction β 2 Grain size segregation in radial F d2 direction F d2 M disk ~ B ~ c2 (T d) 2k 2 T d if, F, = + 2 Measurements for many disks grains are bigger in the inner region Perez et al. (2012)
18 Asymmetry in disks with gaps/holes
19 Credit: NASA; Karen L. Teramura, UH IfA Disks with holes/gaps Williams & Cieza (2011)
20 Large-scale asymmetries Tang et al. (2012), van der Marel et al. (2015), Perez et al. (2014), Marino et al. (2015), Zhang et al. (2014) [ALMA, VLA, PdBI]
21 Gas is less structured General characteristics Gas is present inside the dust cavity but at a reduced level. The outer boundary for the inner cavity 1. Gas radius is smaller 2. Good match between gas & dust Bruderer et al. (2014) Dust ring at AU Gas component starts at 31 AU (Zhang et al. (2014)
22 Extreme asymmetry in dust continuum 440 m Dust cont. 890 m Dust cont. 0.2 van der Marel et al. (2013) Fukagawa et al. (2013)
23 Gas is less asymmetric Bruderer et al. (2014) Fukagawa et al. (2014)
24 van der Marel et al. (2013)
25 Local signature of grain growth Flux ratio is not constant across the disk in azimuthal direction Strong, local grain accumulation and grain growth there Grain size segregation in azimuthal direction. -- Dust trap hypothesis Casassus et al. (2015) Vortex!
26 General characteristics Gas is present inside the dust cavity but at a reduced level. The outer boundary for the inner cavity 1. Gas radius is smaller 2. Good match between gas & dust Gas is less structured Bruderer et al. (2013) Roughly consistent with dust trap idea, but Dust ring at AU Gas component starts at 31 AU
27 How about protoplanets? Catching thermal infrared emission ~6 15 Jupiter-mass at ~20 AU 850 micron dust cont. Giant planet at 53 AU ~30 Jupiter-mass at 23 AU (Kraus and Ireland 2012, Quanz et al. 2012,2014, Reggiani et al. 2014)
28 Multiple, nearly symmetric gaps in HL Tau
29 0.1 Myr ALMA partnership (2015) Close et al. (1997)
30 2.9, 1.3, and 0.87 mm with angular resolutions of (10 AU) to (3.5 AU) Gap location 13, 32, ~42, ~50, 64, 74, ~91 AU The presence of orbital resonances. D1:D2:D3:D4 = 1:4:6:8 β <~ 0.8 in the dark lane grain growth? ALMA partnership (2015)
31 Inspired by ALMA results of HL Tau: condensation fronts? Zhang et al. (2015)
32 0.1 Myr Planet formation begins/proceeds/completes faster than we thought? ALMA partnership (2015) Close et al. (1997)
33 Things to look at in the (near) future 1. Improved statistics for over ~100 disks in nearby star-forming regions 2. Circumplanetary disks 3. Planet formation at an age of <~ 1 Myr 4. High angular resolution for boring, Myrold disks What is the dominant mechanism for planet formation?
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