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STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Study of equatorial Spread-F with ground-based large network observations in Asia and Pacific regions Yamamoto Mamoru 1 , Thampi Smitha 1 , Otsuka Yuichi 2 , Tsugawa Takuya 3 , Nagatsuma Tsutomu 3 , Tsunoda Roland 4 1 Research Institute for Sustainable Humanosphere, Kyoto University, 2 Solar Terrestrial Environment Laboratory, Nagoya University, 3 National Institute of Information and Communications Technology, 4 SRI International Equatorial spread F (ESF) is intense ionospheric irregularity that occurs around the geomagnetic equator. It can cause intense scintillation to satellite-ground communications, and serious error in the GPS measurements. The ESF has been a hot research topic of the equatorial/low-latitude ionosphere for long time. However, its day-to-day variability is not well understood. In the southeast Asian region, Japanese researchers developed a network of ground-based observations with the Equatorial Atmosphere Radar (EAR) of RISH, Kyoto University, the ionosonde network SEALION (SouthEast Asia Low-latitude IOnospheric Network) of NICT, and optical instrument network OMTI (Optical Mesosphere Thermosphere Imager) of STEL, Nagoya University. SRI International deploys a VHF radar, an ionosonde and several satellite beacon receivers on Pacific islands. In addition to this, we are deploying a network of the digital satellite beacon receiver named “GNU Radio Beacon Receiver (GRBR)” to fulfill observation gaps. Multi-beam observation of ESF with the EAR have shown strong evidence that occurrence of the ESF is very close to the sunset of F-region at the dip equator. Our GRBR-TEC measurements with C/NOFS from Vietnam and Indonesia successfully showed longitudinal large-scale wave structure of the ionosphere is in good relationship to the ESF occurrence. From 2010 we further expand the network in Asia and Pacific regions, and tackle yet-unknown day-to-day variability of the ESF.
STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 The dynamical response of ozone and temperature in the lower stratosphere to the 11year solar cycle simulated by the CCSR/NIES CCM Yamashita Yousuke 1 , Sakamoto Kei 2 , Akiyoshi Hideharu 1 , Takahashi Masaaki 3 , Nagashima Tatsuya 1 4 , Zhou L. B. 1 2 3 National Institute for Environmental Studies, All Nippon Airways, Atmosphere and Ocean Research Institute, University of Tokyo, 4 LAPC & LAOR, Institute of Atmospheric Physics, Chinese Academy of Sciences The variation of ultraviolet (UV) radiation with the 11-year solar cycle has been suggested to affect temperature and ozone in the upper stratosphere [e.g., Chandra and McPeters, 1994; Marsh et al., 2007]. While, in the lower stratosphere the direct effect of the UV radiation change with the 11-year solar cycle is considered to be small, and the lower stratospheric ozone is possibly affected by the solar cycle forcing and the sea surface temperature (SST) variations through the circulation change [e.g., Kodera and Kuroda, 2002; Austin et al., 2008]. The three dimensional chemistry climate model (CCM) is able to provide better description of these processes than two dimensional model, and it is especially important for explicit calculation of the planetary wave propagation in the extratropics. It is useful to perform sensitivity experiments using a three dimensional CCM to estimate these processes. Here we show the results which exclude the volcanic eruption, because the CCSR/NIES CCM used in this study overestimates the effects of the volcanic aerosol, which causes unrealistically large solar response in the lower stratosphere with the multiple regression analysis. The control run in this study includes the solar cycle forcing and observed SST and excludes the volcanic forcing. The results is that the contribution of the solar cycle forcing to the solar term is about 1% per 100 units F10.7 in ozone concentration solar response and 0.2 K per 100 units F10.7 in temperature solar response in the lower stratosphere. We show that a change in ozone transport may be the main factor for the solar signal of ozone concentration in the lower stratosphere. The magnitudes of ozone and temperature solar responses in the lower stratosphere are smaller than the observations (about 4% in ozone and 0.5 K in temperature) which implies that some other factors such as the SST, may be included in results based on observations. Another sensitivity experiment with observed SST and fixed solar cycle forcing shows a small solar response in the lower stratosphere, suggesting that the interannual variability of the SST could contribute to the solar term in the lower stratosphere through tropospherestratosphere processes and/or have an effect as an artifact of interference due to the insufficient period for analysis.
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scostep 2010 (stp12) - Leibniz-Institut für Atmosphärenphysik an der ...

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