Variations in Mars’ orbit parameters—obliquity, eccentricity, and season of perihelion—alter the latitudinal and seasonal distribution of daylight, which leads to adjustments to the local weather over time. A few of the penalties of those oscillations embrace the collapse of the environment at low obliquity, a possible improve in atmospheric dustiness and cloudiness at excessive obliquity, and the mobilization and redistribution of floor water ice reservoirs in any respect obliquities. We’re engaged on enhancing our illustration of clouds and their radiative results to raised decide the character of orbit-forced local weather change on Mars.
We use the NASA Ames Mars GCM to handle questions regarding orbit-driven local weather change on Mars. Click on the hyperlinks beneath to study our present tasks on this subject.
Lengthy lived ice-covered Hesperian lakes in Gale Crater, Mars
