climate

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Shape of the Tropopause

Earth’s atmosphere includes several distinct layers that can be identified from one another by differences in temperature, chemical composition, density, and other properties. Most of Earth’s weather occurs in the lower layer of the troposphere, with the layer of the stratosphere residing above. The boundary between these two layers is known as the tropopause and shows variation at different latitudes on Earth. A characteristic tropopause shape shows low heights near the poles, high heights near the equator, and a significant jump (or discontinuity) at about 30 degrees latitude. This variation in tropopause height contributes to variations in weather and climate at different latitudes.

We propose an explanation for the shape of the tropopause in our paper published in Journal of the Atmospheric Sciences. Using a computer climate model (a three-dimensional general circulation model), we create a series of climate states that systematically isolate contributions such as moisture or large-scale weather systems. Although differences in moisture have often been cited as the reason for tropopause variation with latitude, we find that large-scale weather systems (known as eddies in fluid dynamics) alone are necessary to create the characteristic tropopause shape. This leads us to suggest that circulation patterns in the stratosphere may actually be a significant contributor to the troposphere. Or to put it another way: weather patterns on the surface of Earth are significantly influenced by processes in the atmospheric layers above.

Cold Oceans on Early Mars

Billions of years ago, the planet Mars appears to have been covered by a liquid water ocean. Geologic evidence of riverbeds, deltas, canyons, and other features in the Martian landscape all suggest that a flowing liquid once meandered on the surface of the red planet. Even so, the fainter young sun at the time, combined with Mars’ orbital distance from the sun, suggests that even a wet early Mars was probably quite chilly.

In a recent paper published in Nature Geoscience, on which I am a co-author, we examine the idea that early Mars featured a cold glacial ocean on its northern hemisphere. This study combines some theoretical climate calculations (which was my contribution) along with a mineralogical analysis to reach this conclusion. In particular, the formation of minerals known as phyllosilicates would have been prevented in a cold ocean, which may explain the scarcity of phyllosilicates observed in the northern martian hemisphere today.

And if oceans did exist on Mars billions of years ago, then perhaps the processes of life also could have arisen in the early history of the red planet. Mars today appears barren and lifeless, but signs of past or present life could very well be lurking beneath the soil. Future Mars missions, and possibly human exploration, will eventually help to uncover this mystery.

My MS paper, “A Revised, Hazy Methane Greenhouse for the Archean Earth”, just appeared in the journal Astrobiology! You can view a PDF of the article on my research page.

We argue that the warm, ice-free climate of the early Earth (2.8 billion years ago) was maintained by a water vapor/carbon dioxide/methane/ethane atmospheric greenhouse effect that offset the ~20% reduction in solar luminosity from the faint young sun. Furthermore, a stabilizing feedback between life and the climate system may have resulted in a thin stratospheric organic haze that maintained above-freezing temperatures and shielded ultraviolet radiation. An excellent write-up of our work is available at The Planetologist.

I’ve given this talk several times over the past couple years, most recently on the Forum for Astrobiology Research (which should eventually be available as a podcast), and it feels good to finally see the paper come out.