Sub-Neptune planets formed in the protoplanetary disk accreted hydrogen-helium (H,He) envelopes. Planet formation models of sub-Neptunes formed by pebble accretion result in small rocky cores surrounded by polluted H,He envelopes, where most of the rock (silicate) is in vapor form at the end of the formation phase. This vapor is expected to condense and rain out as the planet cools. In this Letter, we examine the timescale for the rainout and its effect on the thermal evolution. We calculate the thermal and structural evolution of a 10 M planet formed by pebble accretion, taking into account material redistribution from silicate rainout (condensation and settling) and from convective mixing. We find that the duration of the rainout in sub-Neptunes is on an Gyr timescale and varies with envelope mass: planets with envelopes below 0.75 M rain out into a core-envelope structure in less than 1 Gyr, while planets in excess of 0.75 of H,He preserve some of their envelope pollution for billions of years. The energy released by the rainout inflates the radius with respect to planets that start out from a plain core-envelope structure. This inflation would result in estimates of the H,He contents of observed exoplanets based on the standard core-envelope structure to be too high. We identify a number of planets in the exoplanet census where rainout processes may be at work, plausibly resulting in their H,He contents to be overestimated by up to a factor two. Future accurate age measurements by the PLATO mission may allow for the identification of planets formed with polluted envelopes.
Bibliographical noteFunding Information:
We thank the referee for constructive comments that improved the manuscript. A.V. acknowledges support by ISF grants 770/21 and 773/21. C.W.O. acknowledge support by the National Natural Science Foundation of China (grant no. 12250610189). Figures were plotted using Matplotlib (Hunter 2007).
© The Authors 2023.
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