FM1.7.02 — Tidal Decay and Disruption of Gaseous Exoplanets

Date & Time

Aug 14th at 11:00 AM until 11:20 AM

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Author(s): Brian Jackson1, Phil Arras4, Sarah Peacock3, Kaloyan Penev2

Institution(s): 1. Boise State University, 2. Princeton University, 3. University of Arizona, 4. University of Virginia

Many gaseous exoplanets in short-period orbits are on the verge or are actually in the process of tidal disruption. Moreover, orbital stability analysis shows tides can drive most known hot Jupiters to spiral inexorably into their host stars. Thus, the coupled processes of orbital decay and tidal disruption likely shape the observed distribution of close-in exoplanets and may even be responsible for producing the shortest-period rocky planets. However, the exact outcome for a disrupting planet depends on its internal response to mass loss and variable stellar insolation, and the accompanying orbital evolution can act to enhance or inhibit the disruption process, depending on the geometry of the atmospheric outflow. In some cases, strong stellar insolation can produce a deep radiative zone in a planet's atmosphere, which can also influence the disruption and therefore the orbital evolution. Understanding these coupled processes and making accurate predictions requires a model that includes both the internal and the orbital evolution of the planet. In this presentation, we will discuss our preliminary work on tidal decay and disruption of close-in gas giants using the fully-featured and robust Modules for Experiments in Stellar Astrophysics (MESA) suite, the capabilities of which were recently upgraded to model gaseous planets with inert, rocky cores.