Pluto System After New Horizons 2019 (LPI Contrib. No. 2133) 7017.pdf PLUTO’S ATMOSPHERE DYNAMICS: HOW THE NITROGEN HEART REGULATES THE CIRCULATION. T. Bertrand1, F. Forget2, A. Toigo3, D. Hinson4,5, 1Space Science Division, NASA Ames Re- search Center Moffett Field, CA 94035, USA (
[email protected]), 2Laboratoire de Météorologie Dy- namique, IPSL, CNRS, Sorbonne Université, Paris, France (
[email protected]), 3Johns Hopkins University Ap- plied Physics Laboratory, Laurel, MD 20723, United States (
[email protected]), 4Carl Sagan Center, SETI Institute, Mountain View, CA 94043, USA,5Department of Electrical Engineering, Stanford University, Stanford, CA 94305, USA (
[email protected]) Introduction: Pluto’s tenuous atmosphere is main- many Pluto years in order to be insensitive to the initial ly nitrogen and is in solid-gas equilibrium with the sur- state, which requires significant computing time. To face nitrogen ice [1]. Over the past three decades, solve this issue, a volatile transport model of Pluto is Earth-based stellar occultations have been an effective used to create initial states for the GCM which are the method to study the evolution of its temperature, com- results of 30 million years of volatile ice evolution and position, pressure, and density [e.g. 2-7]. In particular, contain equilibrated combinations of surface condi- these datasets revealed (1) a much warmer atmosphere tions, such as soil temperatures and ice distributions (70-100 K) than the surface (40 K), with a strong in- [23]. This approach enables 3D GCM simulations of version in the first 20 km above the surface, (2) a three- Pluto to be performed typically from 1984 to 2015, the fold increase of surface pressure since 1988, and (3) first 20 years corresponding to a spin-up time for the global-scale oscillations in the vertical density and atmosphere.