grain surface models and data for astrochemistry
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grain surface models and data for astrochemistry
space Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistryberts1-4 • I). Semenov5 • R.T. Garrod6 7 • E.M. Penteado* • s. loppolo"Received: 8 June 2016/ Accepted: 16 November 2016© The Author(s) 2017. This article is published with open access at springcrlink.comAbstract The cross-disciplinary field of astrochemistry exists to understand the formation, dest grain surface models and data for astrochemistryruction, and survival of molecules in astrophysical environments. Molecules in space are synthesized via a large variety of gas-phase reactions, and rgrain surface models and data for astrochemistry
eactions on dust-grain surfaces, where the surface acts as a catalyst. A broad consensus has been reached in the astrochemistry community on how to suspace Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistryenIE3 H.M. Cuppenh.cuppen@science.ru.nlc. Walshc.Walsh 1 @ leeds.ac.ukT. Lambertslambcrts@thcochcm.uni-stuttgari.deD. Semenovscmcnov@mpia.dcR.T. GarrodrgaiTod@viiginia.edus.loppoloscrgio.ioppolo@opcn.ac.uk1Institute lor Molecules and Materials. Radboud University Nijmegen. Hcycndaalscwcg 135. 6525 A grain surface models and data for astrochemistryJ Nijmegen, The Netherlands2Leiden Observatory. Leiden University. PO Box 9513. 2300 RA Leiden. The NetherlandsSchool of Physics and Astronomy. Univergrain surface models and data for astrochemistry
sity of Leeds, Leeds LS2 9JT. UK4Computational Chemistry Group. Institute for Theoretical Chemistry. University of Stuttgart, pfaffenwaldring 55. 7056space Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistrynia. McCormick Road. PƠ Box 400319. Charlottesville. VA 22904, USA ’7Department of Physical Sciences. The Open University, Walton Hall. Milton Keynes MK7 6AA. UKH.M. Cuppen et al.reached for grain-surface processes. A team of ~25 experts covering observational, laboratory and theoretical (astro )che grain surface models and data for astrochemistrymistry met in summer of 2014 at the Lorentz Center in Leiden with the aim to provide solutions for this problem and to review the current state-of-thegrain surface models and data for astrochemistry
-art of grain surface models, both in terms of technical implementation into models as well as the most up-to-date information available from experimespace Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistrys • Molecular ices • Accretion • Desorption • Photoprocesses • Diffusion1 IntroductionThe very presence of anything but atoms and obscuring minuscule dust grains in the interstellar medium (ISM) was inconceivable by astronomers merely a hundred years ago. Even the brightest minds of the time, such a grain surface models and data for astrochemistrys Sir Arthur Eddington, were doubtful about the existence of molecules in the vast interstellar void. In his Bakerian lecture he pointed out that “...grain surface models and data for astrochemistry
it is difficult to admit the existence of molecules in interstellar space because when once a molecule becomes dissociated there seems no chance of tspace Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistryecies. CN. CH. and CH+. were identified (Swings and Rosenfeld 1937; McKellar 1940; Douglas and Herzberg 1941). The rapid development of radio and infrared detectors following World War II has since allowed the discovery of M90 molecules in the ISM. as of March 2016 (see http://www.astro.uni-koeln.de grain surface models and data for astrochemistry/cdms/molecules). These interstellar species have a multitude of orbital electronic configurations and include stable molecules, radicals, open-shellgrain surface models and data for astrochemistry
molecules, cations, and anions.Many interstellar molecules are recognizable from terrestrial and atmospheric chemistry. Among those are relatively staspace Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistry complex, hydrogen-rich saturated organic molecules are also present in space, e.g., formaldehyde (H2CO). glycolaldehyde (HCOCH2OH), methanol (CH3OH), formic acid (HCOOH), and dimethyl ether (CH3OCH3) (Ehrenfreund and Charnley 2000; Herbst and van Dishoeck 2009). These species “bridge the gap" betwe grain surface models and data for astrochemistryen the simple species listed previously and those considered of prebiotic and biological importance, e.g., amino acids. Other interstellar molecules agrain surface models and data for astrochemistry
re more exotic and unique to space. These include highly-unsaturated carbon chains and cages, e.g.. HC||N (Bell el al. 1997), and the fullerenes. CóQ.space Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistryate in the ISM. Even larger macromolecules. polyaromatic hydrocarbons (PAHs). consisting of between tens and hundreds of carbon atoms, are identifiable in space as a distinct class of species through their characteristic infrared bands (see the review by Tielens 2008). In summary, it is now known th grain surface models and data for astrochemistryat the interstellar matter out of which stars and planets form has a substantial molecular component, w hich plays a pivotal role in the thermal balangrain surface models and data for astrochemistry
ce of the ISM and its evolution (Tielens 2010).The first theoretical models that successfully explained the presence and abundances of early observed space Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. Lamb grain surface models and data for astrochemistryter significantly extended. The common perception in modern astrophysics is that many interstellarReview of Surface Chemistry and Modelsspace Sci RevDOI 10.1 (X)7/s 11214-016-0319-3iJPI^ CrossMarkGrain Surface Models and Data for AstrochemistryH.M. Cuppen' Q • c. Walsh* 1 2-3 • T. LambGọi ngay
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