The first would use the greenhouse effect with radiation from the star and this would create a 'habitable zone' of a few au, with some photon flux from the star reaching the surface albeit not as much as on earth. This also has to do with the two theoretical habitable hydrogen planets that were proposed in literature. In any case the formation + evolution path needs to be different than any planet that we can currently observe and I hope to work and improve on this during the project. Maybe this can lead to cases where the planets are of a few earth masses but have the same metallicity as solar system gas giants. What I would like to try in the future is to see if I can simulate atmosphere loss by collisions. Then for the very small, cold object in our solar system (like Pluto, I don't know if this scale is still relevant in the trend) Jeans escape would be much higher than the planets I simulate. I would argue that the exoplanets that we observe which have a mass of a few earth masses receive a lot more atmosphere loss by radiation that discriminates the lighter hydrogen. I think in this case it's even more important to improve on how I treat condensibles as their actual role could be more different from my simulations.įor the emperical trend between mass and metallicity, I don't think I would necessarily want to go as far as extrapolate the trend to the masses that I'm using for example. This does have some effect on the relation between the duration and the equilibrium temperature + envelope mass, but not a very drastic one. However, currently increasing the metallicity in my case means just increasing the opacities. I did the same first to compare, then added some metals as solar composition, and also ran the same simulations for 10x and 100x solar metallicity. Previous work was with a composition of only hydrogen or hydrogen + helium. The initial motivation was to simulate the greenhouse effect of just hydrogen and see how it behaves alone. Yes I do expect the metallicity of these planets to be/become higher than solar. Thank you for the questions and comments! regarding moist convection in H2-rich atmospheres, an effect that may be very important to consider (or at least, to think about) is the inhibition of convection by the molecular weight vertical gradient caused by water condensation (see ) regarding the possibility to simulate H2-rich atmospheres in 3-D on temperate low-mass planets, I recommend you to read the recent paper:
(2) On your log(ENV)/distance(AU) diagram, wouldn’t you expect (for distance typically larger than 10 AU) that the amount of photons that reach the liquid water ocean is so low (due to both the low insolation and the thickness of the atmosphere that absorb/scatter photons) that phototrophic life would be prevented? Based on the empirical trend (see e.g., ), don’t you expect higher metallicity atmosphere to be more common around low mass planets? (1) What is the motivation for considering solar metallicity atmosphere for such low mass planets? (and not higher metallicity). Hi Marit, Thank you for your presentation! I have several questions: To view this video please enable JavaScript, and consider upgrading to a web browser that supports HTML5 video Ask your questions to Guillaume!
Investigating the runaway greenhouse effect with 1D/3D climate modeling Marit Mol Lous: A water ocean beneath a solar composition atmosphere?Įleonora Alei: Bayesian retrieval for terrestrial atmospheres and interiorsĮmeline Bolmont: Atmosphere-interior interactions impact on orbital/rotational tidal dynamics Noah Jäggi: Mercury's Earliest Atmosphere Martin Turbet: Why and when high molecular mean atmospheres have an impact on mass-radius relationshipsĭeniz Soyuer: The interplay between composition, zonal flows and magnetic fields in Uranus and Neptune Guillaume Chaverot: Investigating the runaway greenhouse effect with 1D/3D climate modeling You can leave questions below the video of each speaker! These questions will then be asked to the speaker the day of the workshop. Please find below the talks of people who work mainly on the atmosphere of planets.