Update 2/29

Read the Stone-Proga paper - a comparison of 2D simulations to spherically symmetric simulations run by others. They characterize escape from the planet with the hydrodynamic escape parameter, use no magnetism (hydrodynamic rather than MHD), and ignore heating and small-scale effects at the base of the wind.

In models with no stellar wind and an isothermal outflow, they find that the sonic surface of the wind is closer to the planet, with a slower radial velocity on the night side of the planet, and a very evident shock in the |v|/vs plot at various angles. For larger values of gamma, this shock produces a delta T, and the sonic surface is farther from the planet (but still nearer than in the spherically symmetric models). Introducing a stellar wind creates a back-swept profile, but has little effect on the sonic surfaces or mass-loss rate.

Should have more time to read Murray-Clay and a few other papers this week.

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