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The World Space Observatory for UV (WSO/UV): implications for solar system studies Isabella Pagano, Giuseppe Leto, Salvatore Scuderi, Giovanni Strazzulla INAF, Catania Astrophysical Observatory, Italy Noah Brosch The School of Physics and Astronomy, Beverly and Raymons Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel Norbert Kappelmann Institut für Astronomie und Astrophysik, Eberhard Karls Universität Tübingen Boris Shustov Institute of Astronomy of the Russian Academy of Science and the WSO/UV Implementation Committee Primary Mirror Unit Optical Bench Mounting Unit Imager Unit Optical Bench Guiding Sensor Launch and Launcher v Launch is scheduled for the end of 2010. v. The Zenith 2 E with booster Fregat will be used to deliver the S/C in vicinity the Lagrangian point L 2. Sky visibility in 5 years from L 2 Lagragian orbit The Jupiter aurora in the UV with the HST/STIS. The three pictures below show the evolution of spatial resolution offered by HST in observing the Jupiter aurora. The HST/STIS MAMA image is the only one showing the trail of the Io magnetic footprint below the auroral oval (from Gerard et al. 2003 http: //lpap. astro. ulg. ac. be/jupiter). The continuum spectrum of comets below 300 nm has rarely been studied. The spectrum seems to be solar, with a slope of order 10% per 100 nm near 290 nm. For further information contact: Prof. Boris Shustov, [email protected] ru (Project PI) Dr. Isabella Pagano, [email protected] inaf. it (FCU PI) Dr. Norbert Kappelmann, [email protected] uni-tuebingen. de (HIRDES PI) A low resolution ( 6 Å) IUE spectrum of comet Hyakutake. WSO/UV with HIRDES will be capable to deliver high-res spectra (R 50, 000) of similarly bright comets. Detailed observations of the UV spectrum of periodic comets are still to be made. One expects, due to a very different thermal history, that the spectrum of periodic comets would be severely depleted in some highly volatile species, e. g. , CO. This can be tested by detecting and monitoring the emissions of CO and CO 2, or those of C and O when the former are not detected.