Concluding remark Yasuhiro Hasegawa (EACOA Fellow @ NAOJ)

Our starting points

Exoplanet observations

ALMA observations

Our starting points

Exoplanet observations

ALMA observations

Planet formation

Star formation Astrobiology

Clumps/Class 0 Class I envelope

Day 1: Formation of circumstellar disks

Theory: consensus is not fully obtained Problems : magnetic breaking, : treatment of sink particles(inner boundary) Promising ideas: formation of first cores (dead zones), : dissipation of envelopes

Observations:

Clumps/Class 0 Class I envelope

Day 1: Formation of circumstellar disks

Theory: consensus is not fully obtained Problems : magnetic breaking, : treatment of sink particles(inner boundary) Promising ideas: formation of first cores (dead zones), : dissipation of envelopes

Observations: 50-100 AU-sized, Keplerian disks are observed : detection of various molecules gives clues of how disks form : detection of larger (~ mm) grains

Clumps/Class 0 Class I Class IIenvelope

Day 2: Protoplanetary disks (including HL Tau)

Theory: Chemistry, gas dynamics, & planet formation are all the important ingredients in understanding disk properties

Chemistry => ice lines, the composition of planets & comets, etc gas dynamics (instabilities) & disk-planet interactions => disk structures such as gaps & spirals

Observations:

Clumps/Class 0 Class I Class IIenvelope

Day 2: Protoplanetary disks (including HL Tau)

Theory: Chemistry, gas dynamics, & planet formation are all the important ingredients in understanding disk properties

Chemistry => ice lines, the composition of planets & comets, etc gas dynamics (instabilities) & disk-planet interactions => disk structures such as gaps & spirals

Observations: disk mass (gas & dust), the stellar mass dependence, molecules : grain growth, chemistry, next-generation of telescopes

Clumps/Class 0 Class I Class II Planetary Systemsenvelope

Day 3: Formation & Evolution of Planets

Theory: Core accretion vs GI (planetesimal-induced migration, thermal evolution of planetesimals, collisions and debris disks) : orbital evolution of planetary systems (scattering vs migration)

Observations:

Clumps/Class 0 Class I Class II Planetary Systemsenvelope

Day 3: Formation & Evolution of Planets

Theory: Core accretion vs GI (planetesimal-induced migration, thermal evolution of planetesimals, collisions and debris disks) : orbital evolution of planetary systems (scattering vs migration)

Observations: SEEDS project (direct-imaging) : radial velocity & occurrence rate of planets : transit & dynamical history of planetary systems

Clumps/Class 0 Class I Class II Planetary Systemsenvelope

Day 4: Atmospheres + future missions + Astrobiology

Theory: super-Earths & sub-Neptunes : interior modeling & evolution of planetary atmospheres (presence of water in the atmosphere)

Observations:

Clumps/Class 0 Class I Class II Planetary Systemsenvelope

Day 4: Atmospheres + future missions + Astrobiology

Theory: super-Earths & sub-Neptunes : interior modeling & evolution of planetary atmospheres (presence of water in the atmosphere)

Observations: Kepler mission (mass-radius diagram) : transmission spectroscopy (instrumental noises) : the composition of atmospheres (water, clouds, haze) : characterization, habitability, biomarkers : K2 + TESS + PLATO + TMT + CHEOPS + JWST

Key next questions??

MY Key questions (highly biased)

Clumps/Class 0 Class I Class II Planetary Systemsenvelope

Grain Growth (coupled with Chemistry)

Clumps/Class 0 Class I Class II Planetary Systemsenvelope

Grain Growth (coupled with Chemistry)

Disk Evolution

Clumps/Class 0 Class I Class II Planetary Systemsenvelope

Grain Growth (coupled with Chemistry)

Disk Evolution

Composition of Planets

Acknowledgements

All the participants: 8 from overseas : 57 from Japan

SOC/LOC: Nakamura-san, Fukagawa-san, Omiya-san, Wakita-san, Shibata-san, Onitsuka-san,

Tatsuuma-san

Funding sources: DTA @ NAOJ & EACOA grant