We present a new code for the study of planetary atmospheres. In recent years there have been a number of newly developed numerical techniques of the study of these systems. Each code has its own strengths and peculiarities. The PATMO code has been designed to specifically account for photo-chemically induced and chemically affected atmospheric compositions. To achieve this task, the code solves chemical production, depletion and transport in a 1D framework. In order to make this model applicable to a wide range of planetary systems, it is built to account for ultraviolet light absorption opacities, first and second kinetic rate reactions with an option to pressure dependent reactions, and reverse chemistry with equilibrium constants calculated with NASA polynomials. The boundary conditions for a geochemical model require the solar flux from the parent star, gravitational constant, and the flux of material into the atmosphere. Based on this information the model computes transport, deposition, chemistry, radiative transfer and optical opacity of the atmosphere (currently only in the UV). The ability to reproduce the chemical composition of a given planet resides on the resolution of large networks of chemical reactions coupled to transport and deposition. The extent of the chemistry included in an Earth like planet can be limited to hydrogen and the Carbon, Nitrogen, Oxygen and Sulfur cycles. Regardless of the reducing or oxidizing conditions of an atmosphere the chemical combinations of these elements are vast and each reaction requires specific kinetic data. Furthermore, the photochemistry associated to the incoming UV solar flux requires molecule specific absorption cross sections. The PATMO model is a 1D photochemical model capable to account for most of the above boundary conditions and in its current state is being used to estimate chemical networks of the main element cycles (C, N, O, H and S). We present a series of results that help to validate and benchmark the model. In this talk we present the results of the Sulphur cycle in the present atmosphere, expanded to the pre-industrial revolution, and the Archean Earth.
Unless announced otherwise, the lunch talks start at 12:50 sharp. The approximate duration of the lunch talk is given above, and additional time will be given for questions and discussion following the presentation. Please make sure that you take ample time to pick up your lunch beforehand.
Information for Speakers and Hosts: Talks are limited to 25 minutes, with 5 additional minutes for questions. Hosts are responsible for bringing the speaker to the correct room in ample time to set up laptops etc., and for ensuring the speaker also has time for lunch.
For questions and/or suggestions concerning the lunch talks, please contact Themiya Nanayakkara () or Alvaro Hacar ()).