ACP Atmospheric Chemistry and Physics ACP 1680-7324 Copernicus GmbH Göttingen, Germany 10.5194/acp-11-9089-2011 Composition changes after the "Halloween" solar proton event: the High Energy Particle Precipitation in the Atmosphere (HEPPA) model versus MIPAS data intercomparison study Funke B. 1 Baumgaertner A. 2 Calisto M. 3 Egorova T. 4 Jackman C. H. 5 Kieser J. 6 Krivolutsky A. 7 López-Puertas M. 1 Marsh D. R. 8 Reddmann T. 9 Rozanov E. 3 4 Salmi S.-M. 11 12 Sinnhuber M. 9 10 Stiller G. P. 9 Verronen P. T. 11 Versick S. 9 14 von Clarmann T. 9 Vyushkova T. Y. 7 Wieters N. 10 Wissing J. M. 13 Instituto de Astrofísica de Andalucía, CSIC, Granada, Spain Max Planck Institute for Chemistry, Mainz, Germany Institute for Atmospheric and Climate Science ETH, Zurich, Switzerland Physical-Meteorological Observatory/World Radiation Center, Davos, Switzerland NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Max Planck Institute for Meteorology, Hamburg, Germany Central Aerological Observatory (CAO), Dolgoprudny, Moscow Region, Russia National Center for Atmospheric Research, Boulder, CO, USA Karlsruhe Institute of Technology, Institute for Meteorology and Climate Research, Karlsruhe, Germany Institute of Environmental Physics, University of Bremen, Bremen, Germany Earth Observation Unit, Finnish Meteorological Institute, Helsinki, Finland Department of Physics, University of Helsinki, Helsinki, Finland FB Physik, University of Osnabrück, Osnabrück, Germany Steinbuch Centre for Computing, Karlsruhe, Germany 05 09 2011 11 17 9089 9139 This is an open-access article ditributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited. This article is available from http://www.atmos-chem-phys.net/11/9089/2011/acp-11-9089-2011.html The full text article is available as a PDF file from http://www.atmos-chem-phys.net/11/9089/2011/acp-11-9089-2011.pdf

We have compared composition changes of NO, NO<sub>2</sub>, H<sub>2</sub>O<sub>2</sub>, O<sub>3</sub>, N<sub>2</sub>O, HNO<sub>3</sub>, N<sub>2</sub>O<sub>5</sub>, HNO<sub>4</sub>, ClO, HOCl, and ClONO<sub>2</sub> as observed by the Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) on Envisat in the aftermath of the "Halloween" solar proton event (SPE) in late October 2003 at 25–0.01 hPa in the Northern Hemisphere (40–90° N) and simulations performed by the following atmospheric models: the Bremen 2-D model (B2dM) and Bremen 3-D Chemical Transport Model (B3dCTM), the Central Aerological Observatory (CAO) model, FinROSE, the Hamburg Model of the Neutral and Ionized Atmosphere (HAMMONIA), the Karlsruhe Simulation Model of the Middle Atmosphere (KASIMA), the ECHAM5/MESSy Atmospheric Chemistry (EMAC) model, the modeling tool for SOlar Climate Ozone Links studies (SOCOL and SOCOLi), and the Whole Atmosphere Community Climate Model (WACCM4). The large number of participating models allowed for an evaluation of the overall ability of atmospheric models to reproduce observed atmospheric perturbations generated by SPEs, particularly with respect to NO<sub>y</sub> and ozone changes. We have further assessed the meteorological conditions and their implications for the chemical response to the SPE in both the models and observations by comparing temperature and tracer (CH<sub>4</sub> and CO) fields. <br><br> Simulated SPE-induced ozone losses agree on average within 5 % with the observations. Simulated NO<sub>y</sub> enhancements around 1 hPa, however, are typically 30 % higher than indicated by the observations which are likely to be related to deficiencies in the used ionization rates, though other error sources related to the models' atmospheric background state and/or transport schemes cannot be excluded. The analysis of the observed and modeled NO<sub>y</sub> partitioning in the aftermath of the SPE has demonstrated the need to implement additional ion chemistry (HNO<sub>3</sub> formation via ion-ion recombination and water cluster ions) into the chemical schemes. An overestimation of observed H<sub>2</sub>O<sub>2</sub> enhancements by all models hints at an underestimation of the OH/HO<sub>2</sub> ratio in the upper polar stratosphere during the SPE. The analysis of chlorine species perturbations has shown that the encountered differences between models and observations, particularly the underestimation of observed ClONO<sub>2</sub> enhancements, are related to a smaller availability of ClO in the polar night region already before the SPE. In general, the intercomparison has demonstrated that differences in the meteorology and/or initial state of the atmosphere in the simulations cause a relevant variability of the model results, even on a short timescale of only a few days.

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