Time: a new dimension of constraints for planet formation and evolution theory

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1 S. Jin, P. Mollière Max Planck Institut for Astronomy, Heidelberg, Germany Y. Alibert & W. Benz University of Bern, Switzerland Christoph Mordasini PLATO meeting Taormina Time: a new dimension of constraints for planet formation and evolution theory

2 Adding the temporal dimension with PLATO Rauer et al Stellar masses and ages will be tightly constrained by the systematic use of asteroseismology. Ages will be known to % for solar-like stars. For the first time with PLATO: population-wide and accurate planet evolution in time as a measurable quantity on the observational side On the theoretical side: temporal evolution: a fundamental and omnipresent concept

3 Radius evolution and formation Radius evolution in time depends on Implication for planet formation initial thermodynamic state (how hot initially / entropy) Bulk composition (H/He, silicates, Fe, ices) Energy transport in the interior (convection) Atmosphere & opacity (Giant) planet formation mode, gas accretion shock structure Formation location, migration, opacity in the protoatmosphere, planetesimal / pebble accretion Accretion history, planetesimal size Enrichment, formation location Atmospheric escape/evaporation Efficiency of H/He accretion Bloating mechanisms Migration mechanism (Kozai, disk migration) New constraints to better understand planet formation

4 Temporal evolution: giant planets Fortney et al Atmospheric model Inflation Guillot & Showman 2002 Leconte & Chabrier 2013 Energy transport Composition Init. cond. Mordasini 2013

5 Temporal evolution low-mass planet Mini-Neptune a=0.05 AU Mcore=4 MEarth Menv=0.1 MEarth Linit=0.1 LJ Earth-like core (0.33 iron, 0.66 silicate) X-rays & EUV evaporation Solar-composition opacity Radius [Earth radii] total radius w/o evap total radius w/ evap core radius Envelope Mass [Earth masses] Venus atmosphere mass Envelope mass Time Time since since disk formation dissipation [Myr] [Myr] Time Time since since disk formation dissipation [Myr] [Myr] -fast decrease from ~2 REarth to R=Rcore when envelope totally lost All these R(time) curves are not directly observationally constrained

6 Mstar=1 Msun, isothermal type I migration rate x 0.1, cold accretion. 1 embryo/disk, no special inflation mechanisms. Temporal evolution of the a-m diagram Output of core accr. population synthesis Only thermodynamic evolution Not dynamics Thermodynamic evolution (cooling & contraction) in time w. atmos. escape Close-in, low-mass loose the envelope. Most of the action early on. Jin et al Black: Bare rocky cores a-m does not change much. (a>0.06 AU)

7 Mstar=1 Msun Isothermal Type I rate x 0.1. Cold accretion. 1 embryo/disk, no special inflation mechanisms. Temporal evolution of the a-r diagram Artifact of using Mmin=1 MEarth a-r does change! -Contraction -Evaporation -Empty valley below 1-2 REarth Black: Bare rocky cores

8 Radius distribution as a function of time 0.1 Gyr 1 Gyr Gyr Radius distribution as function of time: Key constraint for planet formation and evolution theory and Observed version by PLATO come back in 2030 :-) Have this in 2030 not from theory, but from PLATO data! 2 Radius alone sufficient No mass needed

9 Transition solid - gas rich planets Kepler: numerous close-in small planets: 49% of stars (P<0 d, R<4 R Earth ) Many are low-density planets (likely with a few percent of H/He) Important for formation theory, but also habitability At which mass and orbital distance is the transition? In principle simple solution with time dimension: Solid planets: mean density ~constant in time Not only giants planets Gaseous planets: mean density increases: contraction, evaporation Comparison with spectroscopy and dynamics of multiple planet systems

10 Transition solid - gas rich planets Equilibrium temperature Search for the 900 transition in the 800 M-rho-t space exoplanets.org cf. Rauer et al ce i re u P Gyr 0.1 Gyr Gyr rth a E like 500 Mean density [g/cm 3] 3 Mean density [g/cm ] 3 Planetary Density [Grams/Centimeters ] exoplanets.org 11/1/ [Earth Mass]00 Msin(i) 0 00 Mass [Earth masses] Mass [Earth masses] 1 Msun star. Initial conditions from population synthesis Giants: hotter less 500 dense: bloating Low mass: hotter 200 denser: evaporation

11 Origin of close-in low-mass planets Essential open question for planet formation theory Rapid migration from beyond the iceline: ice-rich interior In situ formation or slower migration: rocky interior Mass-radius relation degenerate: iron/silicate/ice/h-he If we can rule out (observationally) that a subpopulation of planets can have a significant H/He atmosphere, break degeneracy

12 Origin of close-in low-mass planets Synthetic Observation Marcy et al Planets with density of 2-3 g/cm 3 in the static part of the a-r (no time evolution i.e. no H/He envelope) must be icy

13 Conclusions -PLATO s ability to accurately determine the ages of the host stars adds a new class of constraints for formation theory -With the time dimension, it should become possible to observationally see -the transition from solid to gas-rich planets -the composition of close-in low-mass planets -This constrains several key concepts of planet formation theory like -efficiency of H/He accretion -orbital migration -The mass is sometimes not necessary for these new constrains: the radius and the age are sufficient

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