Thermal evolution of an early magma ocean in interaction with the atmosphere : conditions for the condensation of water ocean
type: Dataset
description: The research of new life forms is an exciting quest but requires understandingthe origin of the appearance of a form of life. The only planet that houses life as weknow is the Earth. Understand why the other planets in our solar system do nothouse it, is needed to better target our looking for new lives in other star systems.The objective of this thesis is to provide preliminary answers to this question.We mainly focused on the comparison between thermal evolution of Mars, Earthand Venus to the end of their accretion during their cooling magma ocean. Thethermal evolution of magma oceans produced by collision with giant impactorsduring accretion is expected to depend on the composition and structure of theatmosphere through the greenhouse effect of CO2 and H2O released by the magmaduring its crystallization. In order to constrain the various cooling timescales ofthe system, we developed a 1-D parameterized convection model of a magma oceancoupled with a 1-D radiative-convective model of the atmosphere. We conducted aparametric study and described the influence of several variables such as the initialvolatile inventories, the initial depth of the magma ocean and planet-sun distance.Our results suggest that the presence of a steam atmosphere delays the end ofthe magma ocean phase by about 1 Myr. In addition, we also observe that thewater vapor condenses to an ocean after 0.1, 1.5 and 10 Myr respectively for Mars,Earth and Venus. This time would be virtually infinite for an Earth-sized planetlocated at less 0.66 UA from the sun. In view of these results, we note that for theEarth and Mars, the timescales of the water ocean formation are shorter than timegaps between major impacts. This would imply that successive water oceans mayhave developed during accretion. However, Venus, due to its close proximity to thethreshold distance from the sun (0.66 AU), could have maintained its magma oceanphase longer during accretion. Thereafter, taking into account the hydrodynamicesca…
landing page: https://theses.hal.science/tel-00931698
identifier: NNT: 2013PA112285
keyword: eau
keyword: habitabilite
keyword: habitability
keyword: infoeu-reposemanticsdoctoralthesis
keyword: magma
keyword: ocean
keyword: planetary
keyword: planete
keyword: sdustusciences-of-the-universe-physicsearth-sciences
keyword: theses
keyword: water
issued: 2026-05-07T09:40:59.892636
modified: 2026-05-07T09:40:59.892641
language: fr
contact point: Organization
  fn: CCSD

test_moissonnage_selune
type: Agent

Thermal evolution of an early magma ocean in interaction with the atmosphere : conditions for the condensation of water ocean
type: Distribution
format: HTML
access URL: https://theses.hal.science/tel-00931698
issued: 2026-05-07T09:40:59.894987
modified: 2026-05-07T09:40:59.876558