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ARIEL Atmospheric Remote-sensing IR Exoplanet Large-survey (ESA M4 proposal) Towards a statistical description of planets Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 The Solar System is not representative There is much more variety than the Sun’s planets ? Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Key questions Why the Solar System is as it is? is it special? Why are exoplanets as they are? What are the causes for the observed diversity? Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Stars are well behaved…. (Hertzsprung-Russel diagram, 1910) The breakthrough to understanding stars, was the coherent analysis of a large sample and the identification of the most “important” parameters Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Planets are more complex Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Planets are more complex Which are the main properties that determine the characteristics of a planet and its following evolution? ! Planet mass ! Orbital distance ! Formation site ! Stellar luminosity and color ! temperature ! Proto-planetary disk lifetime ! ….. Is it possible a “population” description for planets? Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 How to proceed? • We may select planets according to planet mass, orbital distance stellar, radiation properties (a >3-d grid) • But these parameters are not sufficient ! initial conditions and evolution • Do we have diagnostics reminiscent of initial conditions and planet history? Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Predicted atmospheric composition of exoplanets (2014) – main component Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Forget & Leconte, 2013 Predicted atmospheric composition of exoplanets (2014) – main component Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Forget & Leconte, 2013 Strategy for low mass (warm-hot) planets A >3-d grid to explore 1) planet mass 2) stellar radiation (luminosity & color) 3) Temperature * Few objects per bin – measurement of main components and of equilibrium temperature Minimum requirement #bins 3x3x3=27 bins to explore " >100 targets Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Predicted atmospheric composition of exoplanets (2014) – main component Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Forget & Leconte, 2013 Disks allow planets to migrate ! Migration stops when disks dissipate Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Ariel Carbon/Oxygen Understanding planet formation/migration (~500/1000 planets) 1.2 1.0 0.8 0.6 0.4 0.2 0.0 1 AU 10 AU 100 AU Obert et al., 2011; Turrini, Nelson,Barbieri 2014 Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Massive (warm-hot) planets ! C/O ratio " formation site ! After migration the final distance from the star (temperature) is reached when the disk is dissipated " migration timescale vs disk dissipation time ! The distribution of eq. temperature (final distance from star & chemistry) depends also on the combination of formation site & disk lifetime. Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Main components Equilibrium temperature C/O ! > 500 targets Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Information on Planet mass Stellar radiation Orbital distance Ariel observations Input Strategy for massive (warm-hot) planets Formation site Initial mass Disk lifetime Optimal spectral window (2-8 micron) Hot & warm planets Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Optimal spectral window Molecular signatures 1 micron 2.5 micron 5 micron Water vapour Methane Carbon dioxide Carbon monoxide Ammonia Hydrogen cyanide Ozone Phosphine Hydrogen Sulfide Acetylene Ethane Sulfur Dioxide Titanium Oxide Vanadium Oxide 11 micron H3+ Tinetti, Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Encrenaz, Coustenis, 2013 Targets from NASA-TESS Dedicated mission to detect transiting planets (2017) Transiting planets expected to be discovered by TESS Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014Courtesy of the TESS team Targets from ESA-PLATO Dedicated mission to detect transiting planets (2024) Courtesy of the TESS & PLATO teams Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Requirements ! Bandwidth 2- 8 micron ! Spectral resolution ~200 ! 1m class (70K) ! Compact instrument (50K, 40K detector) ! Low noise ! High throughput ~.35 Initial radiometric model: the case of a warm Neptune @SNR=10, K ~9 CH4 CO CO2 NH3 3.3μ 2.3μ 4.6μ 2.8μ 4.3μ 3.0μ 6.1μ 10-7 10-3 10-5 10-6 10-7 10-6 10-6 Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Current an Ariel observations Equilibrium chemistry Non-equilibrium chemistry ~ 10 planets Today ~ 500-1000 planets Ariel Ariel Ariel Ariel Today Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014 Venot et al., 2012 Venot et al 2012 Atmospheric Remote-sensing IR Exoplanet Large-survey (ARIEL) proposal due to 15 January 2015 Ariel, La ricerca sui pianeti extrasolari in Italia, Roma – 5-7 Novembre 2014