Exoclimes_Conference_booklet1

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non hydrostatic Euler equations on a modified Yin-Yang grid, which consists of an equatorial belt and two polar caps, which are patched together using a fully conservative zonal interface algorithm, described by Wang (1995). The individual grids are solved with a horizontal explicit and vertical implicit (HEVI) finite difference scheme, where the vertical solution can be computed analytically. In this poster we present the implemented scheme and show as well results of the first tests, including a quantification of the conservation of energy, mass and momentum. Compared to other available CPU codes, Thor shows a speed-up of around one magnitude. Thor is written in Cuda C and runs on all Nvidia GPU's. The <strong>Exoclimes</strong> Simulation Platform! Kevin! Heng! — Center for Space and Habitability, University of Bern ! The state of the art in performing 3D simulations of exoplanetary atmospheres centers around adapting GCMs (general circulation models), originally designed for the study of Earth. These Earth-centric tools suffer from fundamental shortcomings, including Earthcentric assumptions, the inability to model shocks, the exclusion of magnetic fields and the treatment of radiative transfer as if the atmosphere is static. We offer an alternative perspective: the design and development of a set of publicly available, theoretical and simulational tools for the general exoplanet community, partly to combat the growing "black box" culture in our field. I give a brief and broad review of the <strong>Exoclimes</strong> Simulation Platform (ESP), focusing on the GCMs and radiative transfer tools that are currently in development. I will also explain our decision to build the ESP entirely on GPUs, which gives our open-source tools a speed-up of at least an order of magnitude (two orders of magnitude for radiative transfer). I will describe how we plan to involve the community via a web portal (www.exoclime.org), which includes a Facebook page for soliciting feedback. VIPER: Toward a universal model for planetary climate Nicolas Iro — University of Hamburg With the discovery of an increasing number of planets outside our Solar System, we are becoming familiar with physical conditions and atmospheric compositions that span a much wider range that what covered by the planets of our solar system. Non-exhaustive examples are equilibrium temperatures ranging from 50K (Neptune) to over 3000K (WASP-12b, WASP18b); orbital eccentricity, ranging from 0-0.1 for solar system planets (except Mercury) and circularized close-in hot Jupiters to e = 0.93 (HD80606b). Other parameters relevant for atmospheric dynamical features are also quite diverse: the Rhines length and Rossby length are, e.g., much smaller than the planet radii for Solar-System planets, while they are comparable to the planetary radii for hot Jupiters and Neptunes, meaning that in the latter case typical circulation features are global. It seems timely and urgent to try to frame in a common framework our understanding of such a large variety of atmospheric conditions. We will present VIPER, the Versatile Interactive PlanetSimulator for Extrasolar Research. This project, under development, aims at developing the Planet Simulator, an already flexible climate model to a new level of modularity. In the next phase of the implementation, we will remove all parameterization pertaining to Earth, allowing for instance to study any planetary rotation rate and add a simple yet precise radiative scheme based on the k-distribution coefficients. This will allow us to model the climate on a variety of planetary conditions from early Mars to Super-Earths. 54
Modelling of the Emission Spectrum of WASP-19b Lucyna Kedziora-Chudczer — University of New South Wales The VSTAR radiative transfer code was used to model the emission spectrum of the one of the most irradiated hot-Jupiters, WASP-19b. We examined models with different pressure-temperature profiles and C/O abundances ratios. We find that models with carbon enrichment above solar match the available data best. We also included upperatmosphere haze of varied particle sizes and find that particles
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PROGRAMME & ABSTRACTS 1
Page 4 and 5: Presentation Venue Davos is a winte
Page 6 and 7: Programme Tuesday 11th Session: Exo
Page 8 and 9: Programme Thursday 13th Session: Br
Page 10 and 11: Participants PARTICIPANTS Dorian! A
Page 12 and 13: Participants Sara! Khalafinejad! Ha
Page 14 and 15: TALKS/POSTERS ABSTRACTS * INSIGHTS
Page 16 and 17: Finally, we will show GCM simulatio
Page 18 and 19: Our results show that whatever the
Page 20 and 21: planets are now available, constrai
Page 22 and 23: sophisticated atmosphere and surfac
Page 24 and 25: Exoplanetary Extreme Space Weather
Page 26 and 27: consistently calculates the ground
Page 28 and 29: pressure.The Bcool project is an in
Page 30 and 31: the climate on exoplanets by provid
Page 32 and 33: new inversion framework for the int
Page 34 and 35: combined observations provide const
Page 36 and 37: Constraining the degeneracy of Supe
Page 38 and 39: structure by integrating the couple
Page 40 and 41: carbon- and oxygen-bearing species.
Page 42 and 43: abundances of molecules in the atmo
Page 44 and 45: data reduction stage crucial to our
Page 46 and 47: us to reproduce this transit asymme
Page 48 and 49: atios, and temperature profiles, th
Page 50 and 51: triple stellar system, and a revise
Page 52 and 53: OH, H2, CO, CO2, CH4, NH3, MgO, MgS
Page 56 and 57: ongoing. This will help us understa
Page 58 and 59: measurements of Planet Beta Pictori
Page 60 and 61: models can still be applied in this
Page 62 and 63: Comprehensive Results from the Weat
Page 64: p m~êëÉåå M RMM=ã pql`hb kpq
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