Over the past fifteen years or so, a new paradigm has emerged in the field of planetary formation : gas disks can form tens of millions of years after the protoplanetary disk has disappeared. This follows the observation of gaseous carbon monoxide in cold debris disks (similar to the Kuiper Belt but more massive).
However, models explaining the presence of gas can be applied to disks closer to their central stars, the (exo)asteroid belts. Initially applied to the solar system, this model provides a robust explanation for the prevalence of water on Earth.
To confirm this scenario and investigate its implications, we have generalized this context to extrasolar systems. We were able to determine under what conditions this type of water vapor disk would be observable and what the masses of water potentially accreted onto inner planets would be.
In this presentation, we will therefore explore the results of this study, focusing in particular on the key role played by the evolution of the central star’s luminosity.
