Observability of evaporating lava worlds

Lava worlds belong to a class of short orbital period planets reaching dayside temperatures high enough melt their silicate crust. Theory predicts that the resulting lava oceans outgas volatile components, attaining equilibrium with overlying vapour. This creates tenuous, silicate-rich atmosphere may be confined permanent planet. The James Webb Space Telescope (JWST) will provide much needed sensitivity and spectral coverage characterise these worlds. In this paper, we assess observability characterisable features by self-consistently modelling atmospheres for all currently confirmed targets having sufficient -stellar (>1500 K). To achieve used outgassed chemistry radiative transfer methods compute temperature–pressure profiles, atmospheric chemical compositions, emission spectra. We explore varying free highly elements, accounting possible evolution. Our models include large number neutral ionic species, as well up-to-date opacities. results indicate SiO 2 infrared are best unique identifiers atmospheres, which detectable using MIRI instrument JWST. Detection two species in would allow strong constraints on thermal structure possibly composition melt. also propose certain example TiO, directly tied different classes melts, revealing surface interior dynamics. Currently, there nearly dozen ideal characterisation JWST, already accepted initial General Observers programme.