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Abstract Terrestrial and sub-Neptune planets are expected to form in the inner (less than 10 au) regions of protoplanetary disks1. Water plays a key role in their formation2,3,4, although it is yet unclear whether water molecules are formed in situ or transported from the outer disk5,6. So far Spitzer Space Telescope observations have only provided water luminosity upper limits for dust-depleted inner disks7, similar to PDS 70, the first system with direct confirmation of protoplanet presence8,9.
Abstract Carbon is an essential element for life but how much can be delivered to young planets is still an open question. The chemical characterization of planet-forming disks is a crucial step in our understanding of the diversity and habitability of exoplanets. Very low-mass stars (less than 0.2 M⊙) are interesting targets because they host a rich population of terrestrial planets.
Authors and Affiliations Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, Maryland, USA Z. Rustamkulov & D. K. Sing Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA D. K. Sing, N. H. Allen & L. Ramos-Rosado Department of Astronomy & Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, 95064, USA S. Mukherjee, A. L. Carter, N. M. Batalha, J. J. Fortney & K. Ohno Johns Hopkins APL, Laurel, MD, USA E. M. May, K. B. Stevenson & J.
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