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041-2011-Abstracts-BOE-III-Crete.Pdf Boreskov Institute of Catalysis of the Siberian Branch of Russian Academy of Sciences, Novosibirsk, Russia Institute of Cytology and Genetics of the Siberian Branch of Russian Academy of Sciences, Novosibirsk, Russia Borissiak Paleontological Institute of Russian Academy of Sciences, Moscow, Russia III International Conference “Biosphere Origin and Evolution” RETHYMNO, CRETE, GREECE OCTOBER 16-20, 2011 ABSTRACTS Novosibirsk, 2011 © Boreskov Institute of Catalysis, 2011 INTERNATIONAL SCIENTIFIC COMMITTEE Alexei Rozanov, Borissiak Paleontological Institute RAS, Moscow, Russia Co‐Chairman Georgii Zavarzin, Institute of Microbiology RAS, Moscow, Russia Co‐Chairman Vadim Agol Moscow State University, Russia Yury Chernov Severtsov Institute of Ecology and Evolution, Moscow, Russia Institute of Protein Research RAS, Pushchino, Moscow region, Alexander Chetverin Russia David Deamer Biomolecular Engineering, School of Engineering, Santa Cruz, USA V.S. Sobolev Institute of Geology and Mineralogy SB RAS, Nikolay Dobretsov Novosibirsk, Russia Mikhail Fedonkin Geological Institute RAS, Moscow, Russia Siegfried Franck Potsdam Institute for Climate Impact Research, Germany V.I. Vernadskii Institute of Geochemistry and Analytical Chemistry Eric Galimov RAS, Moscow, Russia Mikhail Grachev Limnological Institute SB RAS, Irkutsk, Russia Richard Hoover Nasa Marshall Space Flight Ctr., Huntsville, USA North‐Western Scientific Center RAS, St. Petersburg State Sergey Inge‐Vechtomov University, Russia Trofimuk Institute of Petroleum‐Gas Geology and Geophysics Alexander Kanygin SB RAS, Novosibirsk, Russia Astrospace Centre of Lebedev Physical Institute RAS, Moscow, Nikolay Kardashev Russia Józef Kaźmierczak Institute of Paleobiology PAN, Warsaw, Poland Nikolay Kolchanov Institute of Cytology and Genetics SB RAS, Novosibirsk, Russia Trofimuk Institute of Petroleum‐Gas Geology and Geophysics Alexei Kontorovich SB RAS, Novosibirsk, Russia National Center for Biotechnology Information, National Library Eugene V. Koonin of Medicine, National Institutes of Health, Bethesda, USA V.I. Vernadskii Institute of Geochemistry and Analytical Chemistry Mikhail Marov RAS, Moscow, Russia Koen Martens Royal Belgian Institute of Natural Sciences, Brussels, Belgium Koichiro Matsuno Nagaoka University of Technology, Nagaoka, Japan Victor Melezhik Geological Survey of Norway, Trondheim, Norway Sechenov Institute of Evolutionary Physiology and Biochemistry, Yuri Natochin St. Petersburg, Russia Valentin Parmon Boreskov Institute of Catalysis SB RAS, Novosibirsk, Russia Lab. Interuniversitaire Des Systemes Atmopsheriques, Umr Cnrs, François Raulin Paris, France Michael Russell California Institute of Technology, Pasadena, CA, USA N.I. Vavilov Institute of General Genetics RAS, Lomonosov Sergey Shestakov Moscow University, Russia Vladimir Shumnyi Institute of Cytology and Genetics SB RAS, Novosibirsk, Russia Boris Shustov Institute of Astronomy RAS, Moscow, Russia Institute of Protein Research RAS, Pushchino, Moscow region, Alexander Spirin Russia Institute of Chemical Biology and Fundamental Medicine SB RAS, Valentin Vlasov Novosibirsk, Russia Nikolay Yushkin Institute of Geology, UB RAS, Syktyvkar, Russia Lev Zelenyi Space Research Institute, Moscow, Russia LOCAL SCIENTIFIC COMMITTEE Boreskov Institute of Catalysis SB RAS, Valentin Parmon, Co‐Chairman Novosibirsk, Russia Institute of Cytology and Genetics SB RAS, Nikolay Kolchanov, Co‐Chairman Novosibirsk, Russia Valeriy Snytnikov, Boreskov Institute of Catalysis SB RAS, Scientific Secretary Novosibirsk, Russia Sergey Rozhnov Borissiak Paleontological Institute RAS, Moscow, Russia Alexey Lopatin Borissiak Paleontological Institute RAS, Moscow, Russia Boreskov Institute of Catalysis SB RAS, Oxana Taran Novosibirsk, Russia Boreskov Institute of Catalysis SB RAS, Tatiana Zamulina, Secretary Novosibirsk, Russia Conference co‐organizer, executive representative of the Organizing Committee: ILIKO TRAVEL company PLENARY LECTURES PL‐1 EARTH AND PLANETS ORIGIN: HOW DO WE VIEW AND MODEL IT? Marov M. V.I. Vernadsky Institute of Geochemistry and Analytical Chemistry RAS, Moscow, Russia Solar system origin is regarded as a cornerstone of the planets formation and eventually Earth evolution towards biosphere set up. While planets birth from gas‐dust discs is quite routine process in our and other galaxies, solar system configuration, and specifically Earth, seems to be unique. Obviously, multiple physical and chemical processes underlied this event and ensured specific scenario to distinguish solar system from other planetary systems. Understanding and reconstruction of these processes is the main goal and the great challenge of the planetary cosmogony. The contemporary views and further progress in the field are supported by astronomical observations of the numerous gas‐dust discs around young solar type stars, escalating discoveries of extrasolar planets, and computer modeling of the planetary systems formation and early evolution based on the advanced theoretical approach and enormous advancement in computing capacity. Complex problems are addressed in the models development, data of observation placing important constraints on the models validity. Our approach is based on heterogenic mechanics of turbulent media involving in‐depth study of disc thermodynamics on the accretion stage from which the key cosmochemical consequences emerge. In particular we argue that because in the region of Earth‐Venus orbit temperature was not lower than 300– 500 К, the reduced water‐lacking matter different from CI carbonaceous chondrites by absence of hydrosilicates and volatiles would originated. This means that Earth and its neighbors has born as water‐poor bodies and an other source of volatiles, probably of exogenic nature, would require to compensate such a lack and to make possible their hydrosphere/atmosphere appearance. Comets and asteroids impacted inner planets at the very early stage of the solar system formation are invoked as such a plausible source. Disc dynamics is thoroughly evaluated with the involvement of dust subdisk formation in the near‐equatorial plane and its fragmentation into dust clusters due to gravitational instability accompanied by the angular momentum transfer. Numerous solid bodies of asteroid size appeared from subdisk at this early stage within the first million years after solar system formation – evidence that is supported by radio isotopes dating of iron and stony meteorites available as collisional fragments of these bodies which are regarded as the 6 PL‐1 first planetesimals (embryos of planet‐size bodies). The follow up evolutionary dynamics of the protoplanetary disc appears to involve the continuing processes of remaining dust clusters and planetesimals of different size collisions. Basically our dynamical models are focused on the molecular dynamics approach and weighted Monte Carlo algorithms for numerical evaluation of dust clusters formation including coagulation processes and solid bodies interaction under various physical‐chemical parameters and geometry. Peculiarities of gas‐dust clumps interaction with different mass ratio and collision velocities, as well as physical mechanisms occurred in the contact zone of interacting solid bodies involving energy redistribution and some other non‐linear effects were investigated. The models developed allow us to distinguish between the more or less realistic mechanisms of planets grow from planetesimals incorporating chronology emerging from radio nuclides isotopy. Some important questions remain open, however, in particular those about stability maintenance of dust clusters and solid bodies within ring compression, time scale of the processes of interaction and phase transitions including, first of all, condensation and coagulation. These questions and prospects of further study are discussed in terms of their impact on the intriguing problem of life and biosphere origin. 7 PL‐2 ANALYSIS OF ISOTOPE SYSTEM DATA (Hf‐W, Rb‐Sr, J, Pu‐Xe, U‐Pb) AS APPLIED TO THE PROBLEM OF PLANET FORMATION. CASE STUDY: EARTH‐MOON SYSTEM Galimov E.M. V.I. Vernadskii Institute of Geochemistry and Analytical Chemistry RAS, Moscow, Russia Isotope data provide important geochemical constraints for models of accumulation of planets, including the Earth‐Moon system. 182 184 Short living isotope Hf decays into W with T1/2 ~ 9 million years, so that Hf‐W system enlightens the very early stage of accumulation of planets. In particular, analysis of the 182Hf/184W system shows that the Moon could not have come into existence earlier than 50 million years after formation of the Solar system. Since, on the other hand, there are certain rocks on the Moon whose age has been estimated as approximately 70 million years after formation of the Solar system, the Hf‐W system indicates that the likely interval of formation of the Moon would be 50‐70 million years. In contrast to 182Hf 87Rb is a very long living isotope, yielding 87Sr. The lunar initial 87Sr/86Sr suggests some higher Rb content in the Moon than it is observed. Rubidium may have been lost as a volatile element. But because of its high atomic weight, it cannot run away from the lunar surface. Rb may escape only from the heated surfaces of small bodies or particles. It makes likely that the pre‐lunar material existed in a dispersed form at the time preceded to emerging of the Moon as a condensed body (i.e. during about 50‐70 Mln years). Indications on the preliminary dispersed stay may also have been inferred as regard to the Earth accumulation.
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