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STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Effects of solar particle events on the middle atmosphere's chlorine chemistry Winkler Holger 1 , Kazeminejad Shahin 2 , Wieters Nadine 1 , Sinnhuber Miriam 1 , Wissing Jan Maik 3 , Kallenrode May-Britt 3 , Stiller Gabriele 4 , Von Clarmann Thomas 4 , Funke Bernd 5 , Santee Michelle 6 , James M. Russell III 7 1 Institut für Umweltphysik, Universität Bremen, Germany, 2 Deutsches Zentrum für Luft- und Raumfahrt (DLR), Bonn-Oberkassel, Germany, 3 Fachbereich Physik, Universität Osnabrück, Germany, 4 Institut für Meteorologie und Klimaforschung, Karlsruher Institut für Technologie, Germany, 5 Instituto de Astrofisica de Andalucia, Granada, Spain, 6 Jet Propulsion Laboratory, Pasadena, USA, 7 Langley Research Center, USA It is well established that solar proton events (SPEs) are sources of distinct chemical disturbances in the Earth’s polar atmosphere. While the SPE caused production of NOx and HOx and the subsequent destruction of ozone can be reproduced quite well by atmospheric models using basic parameterizations for NOx and HOx release as a function of the particle impact ionization rate, there are significant differences between measurements and model predictions concerning chlorine compounds. Satellite measurements (HALOE, MIPAS, MLS/Aura) have shown that there is also chlorine activation in the stratosphere and mesosphere, and an increase of chlorine nitrate in the lower and middle stratosphere during SPEs. This cannot be explained by the NOx and HOx increase alone. Atmospheric models with standard parameterizations of NOx and HOx production due to SPEs fail to reproduce the magnitude of the observed chlorine disturbances. Numerical simulations using the University of Bremen ion chemistry (UBIC) model show a much better agreement with measurements if full negative ion chemistry is considered additionally to the NOx and HOx production. The UBIC results in combination with atmospheric models indicate that reactions of negative cluster ions can have a significant impact on the middle atmosphere’s chlorine chemistry during SPEs. There is a transformation of HCl into active chlorine via anion cluster chemistry. Additionally, the release of O(1D) through N(2D) + O2 → NO + O(1D) has a considerable impact on chlorine species. Results of UBIC simulations for different SPEs (July 2000, October 2003, January 2005) are presented. They are compared with the observed changes of chlorine compounds – HCl, HOCl, ClO and ClONO2 – from the satellite instruments HALOE, MIPAS and MLS/Aura.
STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Modeling electron density in E- and F-layer: Comparison of the model chain AIMOS- HAMMONIA and ISR measurements Wissing Jan Maik 1 , Kallenrode May-Britt 1 , Kieser Jens 2 , Schmidt Hauke 2 , Rietveld Michael T. 3 , McCready Mary 4 , Erickson Phil 5 1 University of Osnabrück, Barbarastraße 7, 49076 Osnabrück, Germany, 2 MPI Meteorology, Hamburg, Germany, 3 EISCAT Scientific Association, Ramfjordmoen, N-9027 Ramfjordbotn, Tromsø, Norway, 4 Center for Geospace Studies, SRI International, Menlo Park, California, USA, 5 Atmospheric Sciences Group, MIT Haystack Observatory, Westford, MA 01886 USA Ionization due to particle precipitation is the main forcing of the electron density in E- and Flayer during night times. Therefore incoherent scatter radar (ISR) measurements show electron densities exceeding model simulations without particle forcing by up to a factor of 1000. We now implemented a model chain for the Atmospheric Ionization Module OSnabrück (AIMOS), modeling spatially resolved ionization due to particle precipitation, and the climate model HAMMONIA with extended ion chemistry in the E- and F-layer up to approx. 200 km. This presentation will focus on the comparison of modeled electron density in the upper atmosphere and ISR measurements from Sondrestrom, Tromsø, Svalbard and Millstone Hill. As the time period covers October 2003 to April 2004 the results represent geomagnetic quiet as well as active periods (October event 2003). Special interest will also be given to local variations since the ISR stations cover the geomagnetic latitudes from 53 to 76°N. According to the altitude range in this comparison the effect of magnetospheric particles will be discussed in the first instance.
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scostep 2010 (stp12) - Leibniz-Institut für Atmosphärenphysik an der ...

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