Picture a distant world orbiting dangerously close to its host star, its atmosphere slowly bleeding into the cosmic void. This dramatic process of atmospheric escape shapes the exoplanet population we observe today, determining which worlds retain their gaseous envelopes and which are stripped down to rocky cores. Understanding this phenomenon is crucial for explaining the radius gap in the exoplanet population and predicting which planets might harbor stable atmospheres over geological timescales.
Wind-AE transforms this complex astrophysical challenge into a computationally tractable problem. Built on the foundational Murray-Clay et al. (2009) framework, this 1D hydrodynamic code solves the coupled equations of energy conservation, momentum conservation, and ionization equilibrium to model how stellar XUV radiation drives atmospheric outflows. What sets Wind-AE apart is its incorporation of metal physics and multifrequency X-ray capabilities, allowing researchers to explore how heavy elements and high-energy photons influence escape rates. The code employs a Parker wind relaxation method to rapidly compute mass loss rates, velocity profiles, temperature structure, and ionization states throughout the upper atmosphere.
Beyond pure research applications, Wind-AE serves as a powerful tool for connecting theory to observations. Its outputs can be readily translated into predictions for transit observations, including the increasingly important metastable helium absorption signals that reveal atmospheric escape in action. The code’s speed makes it ideal for parameter studies and population synthesis work, while its modular design allows integration with lower atmosphere models for comprehensive planetary atmosphere modeling.
⭐ Stars: 12
💻 Language: Jupyter Notebook
🔗 Repository: mibroome/wind-ae