In this formulation, larger particles denoted as pebbles, feel drag from the gaseous disk and are accreted onto growing protoplanets. The predominant theory to grow these planets is the pebble accretion paradigm. To date, thousands of exoplanets have been discovered a sizeable amount of these planets lie in the intermediate mass range (1-10 Earth masses). Our puzzling findings challenges planet formation paradigms for small planets and we discuss our results in the context of planet formation, comparative exoplanetology with other young and mature systems, as well as within the same system.ĭynamic Disk Temperature and its Effect on Pebbles and Planet FormationĪreli Castrejon (University of Groningen, Kapteyn Astronomical Institute) We find that the planets in this system have lower masses and much lower metal abundances than initially thought, and that atmospheric escape is occurring at lower rates than expected. We present observational campaigns dedicated to probe the atmospheres of the V1298 Tau planets to trace fossil records of their formation, though the determination of their mass, their elemental abundances and metallicity, and ongoing evolution though their atmospheric dynamics and escape. In this context the 23 Myr old V1298 Tau system, composed of three Neptunes/Sub-Neptunes transiting exoplanets, represents a unique opportunity to probe the early conditions of what are most likely super-Earth progenitors. Sub-Neptunes and super-Earths correspond to the most common population exoplanets, yet there are several burning questions regarding their formation and their early evolution. Tracing the late formation and early evolution of young Sub-Neptune progenitors
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