How does chaotic obliquity drive climate evolution on early Mars?
Changes in obliquity affect both the meridional distribution of surface ice and circulation (including cloud formation!). This may lead to dramatic changes in early Martain climate through time.
Can spin provide a new constraint on Venus's atmospheric evolution?
Spin provides a fingerprint of atmospheric evolution through the thermal tide. Can we use Venus's modern rotation rate to rule out proposed evolutionary scenarios?
I explore whether early Venus could have remained habitable as its climate and rotation evolved together. In particular, I study how atmospheric tides, gravitational tides, and clouds may have shaped Venus’s climate trajectory.
How does atmospheric evolution drive spin evolution on rocky planets?
I investigate how atmospheric composition influences planetary rotation through thermal tides. This work explores when rocky planets can maintain asynchronous rotation around small stars.
How do continents affect ocean circulation on tidally locked planets?
I study how the size of continents influences ocean heat transport between the permanent dayside and nightside of tidally locked planets. This work shows how substellar continents can weaken ocean mixing and alter the distribution of surface ice.
How do stratocumulus clouds evolve and affect warm climates on Earth?
I study how low clouds respond to increasing atmospheric CO₂ and warming, using idealized models and climate simulations to understand cloud breakup, multiple climate equilibria, and the implications for past and future warm climates.