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During accretion, the young rocky planets are so hot that they become endowedwith a magma ocean. From that moment, the mantle convective thermal fluxcontrol the cooling of the planet and an atmosphere is created by outgassing.This atmosphere will then play a key role during this cooling phase. Studyingthis cooling phase in details is a necessary step to explain the greatdiversity of the observed telluric planets and especially to assess thepresence of surface liquid water. We used here a radiative-convective 1Datmospheric model (H2O, CO2) to study the impact of the Bond albedo on theevolution of magma ocean planets. We derived from this model the thermalemission spectrum and the spectral reflectance of these planets, from which wecalculated their Bond albedos. Compared to Marcq et al. (2017), the model nowincludes a new module to compute the Rayleigh scattering, and state of the artCO2 and H2O gaseous opacities data in the visible and infrared spectral ranges.We show that the Bond albedo of these planets depends on their surfacetemperature and results from a competition between Rayleigh scattering from thegases and Mie scattering from the clouds. The colder the surface temperatureis, the thicker the clouds are, and the higher the Bond albedo is. We alsoevidence that the relative abundances of CO2 and H2O in the atmosphere stronglyimpact the Bond albedo. The Bond albedo is higher for atmospheres dominated bythe CO2, better Rayleigh scatterer than H2O. Finally, we provide the communitywith an empirical formula for the Bond albedo that could be useful for futurestudies of magma ocean planets.

Modeling the albedo of Earth-like magma ocean planets with H2O-CO2 atmospheres