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Open Research Online Oro.Open.Ac.Uk Open Research Online The Open University’s repository of research publications and other research outputs ESA experiment BIOPAN-6-Germination and Growth Capacity of Lichen Symbiont Cells and Ascospores After Space Exposure Journal Item How to cite: de Vera, J. P.; Ott, S.; de la Torre, R.; Sancho, L. G.; Horneck, G.; Rettberg, P.; Ascaso, C.; de los Ríos, A.; Wierzchos, J.; Cockell, C.; Olsson, K.; Frías, J. M. and Demets, R. (2009). ESA experiment BIOPAN-6- Germination and Growth Capacity of Lichen Symbiont Cells and Ascospores After Space Exposure. Origins of Life and Evolution of Biospheres, 39(3) pp. 359–360. For guidance on citations see FAQs. c 2009 The Authors https://creativecommons.org/licenses/by/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1007/s11084-009-9164-7 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Orig Life Evol Biosph (2009) 39:179–392 DOI 10.1007/s11084-009-9164-7 SPECIAL ISSUE: ABSTRACTS FROM THE 2008 ISSOL MEETING INTRODUCTION TO THE SPECIAL ISSUE This issue of Origins of Life and Evolution of Biospheres contains the abstracts of the scientific contributions presented at the 2008 ISSOL Meeting, which was held in Florence (Italy) on 24–29 August, 2008. The Symposium’s main objectives were to bring together scientists working in different areas of the study of the origin and early evolution of life, to stimulate discussion on this fundamental process and to have an appraisal of the most recent advances in this multidisciplinary field that combines research from space sciences and astrophysics, to chemistry, geology, paleontology, genomics, molecular biology, history and philosophy of science, among others. The meeting was attended by about 350 scientists from all over the world, and more than 310 presentations were given, including 260 posters. This volume collects almost all the contributions, which are an up-to-date account of the state of the knowledge on this exciting area of scientific and educational pursuits. It is with great pleasure that I acknowledge the contributions of different authors in assuring the prompt publication of the OLEB Special Issue. I would also like to express my thanks to the Editor of OLEB, Alan W. Schwartz, and Springer for the publication of the Proceedings. Enzo Gallori University of Florence President of the Local Organizing Committee 180 Orig Life Evol Biosph (2009) 39:179–392 Invited Lectures Search for Potentially Primordial Genetic Systems Ramanarayanan Krishnamurthy The Department of Chemistry at The Scripps Research Institute 10550 North Torrey Pines Road, MB16, La Jolla, CA-92037, USA Extensive base-pairing studies of oligonucleotides consisting of canonical bases tagged to a variety of cyclic sugar-phosphate backbones—conducted in the context of work toward an etiology of the structure type of the natural nucleic acids—have led to a broadening of the scope of investigations to include informational oligomer systems that are not confined to typical sugar-backbones and canonical bases. The lecture will present some recent results: the base-pairing properties of a series of acyclic backbone derived oligomeric systems tagged with alternative heterocycles as recognition elements. E-mail: [email protected] The Formation of Planetary Systems Alan P. Boss Carnegie Institution, Washington DC, USA Planetary systems form out of the leftovers of the star formation process. Dense interstellar clouds of gas and dust collapse under their self-gravity to form central protostars orbited by rotationally supported, flattened disks in which planets later form. The disk that formed the Solar System is called the solar nebula. Terrestrial planets form by the slow process of collisions and sticking between increasingly larger dust grains, pebbles, boulders, and mountains of rock and ice termed planetesimals. Km-size planetesimals are large enough to grow by gravitationally deflecting bodies that might otherwise not collide with them, leading to a period of runaway growth to lunar-sized planetary embryos. The final phase of terrestrial planet formation involves giant impacts between the protoplanets and planetary embryos and requires on the order of 100 million years. While there is a general consensus about the formation of terrestrial planets, two very different mechanisms have been proposed for the formation of the gas and ice giant planets. The conventional explanation for the formation of gas giant planets, core accretion, presumes that a gaseous envelope collapses upon a roughly ten Earth-mass, solid core of rock and ice that was formed by the collisional accumulation of planetary embryos orbiting in the solar nebula. The more radical explanation, disk instability, hypothesizes that the gaseous portion of the nebula underwent a gravitational instability, leading directly to the formation of self-gravitating clumps, within which dust grains coagulated and settled to form cores. Core accretion appears to require several million years or more to form a gas giant planet, implying that only relatively long-lived disks would form gas giants. Disk instability, on the other hand, is so rapid (forming clumps in thousands of years), that gas giants could form in even the shortest-lived disks. Terrestrial planets seem to be likely to Orig Life Evol Biosph (2009) 39:179–392 181 form under either scenario for giant planet formation, though the likelihood does depend strongly on the orbital properties of the giant planets in the system. Core accretion has difficulty in explaining the formation of the ice giant planets, unless two extra protoplanets are formed in the gas giant planet region and thereafter migrate outward. An alternative mechanism for ice giant planet formation has been proposed, based on observations of protoplanetary disks in the Orion nebula cluster and Eta Carina star- forming region: disk instability leading to the formation of four gas giant protoplanets with cores, followed by photoevaporation of the disk and gaseous envelopes of the protoplanets outside about 10 AU by ultraviolet radiation from nearby massive stars, producing ice giants. In this scenario, Jupiter survives unscathed, while Saturn is a transitional planet. The ultraviolet fluxes photoevaporate the outer disk, freezing the orbits of the giant planets, and converting the outer gas giants into ice giants. Because most stars form in regions of high-mass star formation, if this alternative scenario is appropriate for the formation of the Solar System, extrasolar planetary systems similar to our own may then be commonplace. This heretical idea also offers a head start on the formation of prebiotic molecules necessary for the origin of life, as well as a natural explanation for thermally processing primitive materials (chondrules and refractory inclusions) found in meteorites, large scale radial transport of refractories and ices, mixing and homogenization of initially heterogeneous short-lived radioactivities, and transport of stable oxygen isotopes inward from the outer disk surface, as required by cosmochemical constraints on the formation of the Solar System. E-mail: [email protected] Gas-Phase Prebiotic Chemistry in the Solar System: How and Where Nadia Balucani Dipartimento di Chimica, Università degli Studi di Perugia, Perugia, Italy In the sequence of steps which are believed to have led from elementary particles to the emergence of life, an important one is certainly the formation of simple prebiotic molecules from parent species abundant in the Universe. The aggregation of H, O, N, C (and other elements) atoms into molecules and the subsequent chemical evolution are occurring also now in the Universe, as witnessed by the identification of more than one hundred molecules in the interstellar medium (encompassing also prebiotic molecules such as glycolaldehyde, formamide and, tentatively, glycine) and by the gas-phase chemical evolution of the atmospheres of several solar objects like Titan. Simple as they might seem compared to other processes of relevance in astrobiology, the formation mechanisms of many of the observed gaseous prebiotic molecules and radicals are far from being understood. In this contribution, the focus will be on the gas-phase chemical evolution of planetary atmospheres and cometary comae, the gaseous environments of our Solar System where gaseous organic molecules have been observed. Similarly to the atmosphere of Earth, the atmospheres of the other planets (or satellites, like Titan) can be described as giant photo-reactors, where the energy deposited mainly by solar photons, but also by cosmic rays and other energetic particles, drives a complex gas-phase chemistry. In this specific context, gas-phase neutral–neutral reactions are expected to play a dominant role. A thorough characterization of the chemical evolution of planetary atmospheres relies on a multi-disciplinary approach: (1) observations allow us to identify the molecules and their number densities as they are nowadays; (2) the 182 Orig Life Evol Biosph (2009) 39:179–392 chemistry which lies behind their formation starting from atoms and simple molecules is accounted for by complex reaction networks; (3) for a realistic modeling of such networks, a number of experimental parameters are needed and, therefore, the relevant molecular processes should be fully
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