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This would change what the planet's atmosphere looks like from outside.","posed_since":"","precise":"For sub-Neptunes with surface magma oceans at $T \\sim 2000-4000\\,\\mathrm{K}$ under $\\mathrm{H_2}$ envelopes of $\\sim 1-3\\,\\mathrm{percent}$ of the planet mass, determine how $\\mathrm{H_2}$ dissolution into silicate melt and reactions with the melt (FeO and $\\mathrm{SiO_2}$ reduction producing $\\mathrm{H_2O}$, SiO and $\\mathrm{SiH_4}$) set the envelope composition and its mean molecular weight $\\mu$. The answer is predicted $\\mu$ and $\\mathrm{H_2O}$, $\\mathrm{CO_2}$ and SiO abundances versus equilibrium temperature and envelope mass fraction, testable against JWST spectra.","problem_ref":"061d3f762ee73dd15d6422c8431eba2713dde74fb8a7936ae76cd7493a1c29c7","references":"","settled_by":"Coupled magma-atmosphere equilibrium and evolution models that predict the dependence of $\\mu$ on equilibrium temperature, confirmed by JWST spectra of a sample of sub-Neptunes spanning that temperature range.","status_note":"","title":"How do magma oceans change sub-Neptune 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