Synthesis of Activated Pyrimidine Ribonucleotides in Prebiotically Plausible Conditions

Total Page:16

File Type:pdf, Size:1020Kb

Synthesis of Activated Pyrimidine Ribonucleotides in Prebiotically Plausible Conditions Vol 459 | 14 May 2009 | doi:10.1038/nature08013 LETTERS Synthesis of activated pyrimidine ribonucleotides in prebiotically plausible conditions Matthew W. Powner1,Be´atrice Gerland1 & John D. Sutherland1 At some stage in the origin of life, an informational polymer must we have discovered a short, highly efficient route to activated pyrimi- have arisen by purely chemical means. According to one version of dine ribonucleotides from these same precursors that proceeds by way the ‘RNA world’ hypothesis1–3 this polymer was RNA, but attempts of alternative intermediates (Fig. 1, green arrows). By contrast with to provide experimental support for this have failed4,5. In parti- previously investigated routes to ribonucleotides, ours bypasses ribose cular, although there has been some success demonstrating that and the free pyrimidine nucleobases. Mixed nitrogenous–oxygenous ‘activated’ ribonucleotides can polymerize to form RNA6,7,itis chemistry first results in the reaction of cyanamide 8 and glycolalde- far from obvious how such ribonucleotides could have formed from hyde 10, giving 2-amino-oxazole 11, and this heterocycle then adds to their constituent parts (ribose and nucleobases). Ribose is difficult glyceraldehyde 9 to give the pentose amino-oxazolines including the to form selectively8,9, and the addition of nucleobases to ribose is arabinose derivative 12. Reaction of 12 with cyanoacetylene 7 then inefficient in the case of purines10 and does not occur at all in the gives the anhydroarabinonucleoside 13, which subsequently under- case of the canonical pyrimidines11. Here we show that activated goes phosphorylation with rearrangement to furnish b-ribocytidine- pyrimidine ribonucleotides can be formed in a short sequence that 29,39-cyclic phosphate 1. In a subsequent photochemical step, 1 is bypasses free ribose and the nucleobases, and instead proceeds partly converted to the corresponding uracil derivative, and synthetic through arabinose amino-oxazoline and anhydronucleoside inter- co-products are largely destroyed. mediates. The starting materials for the synthesis—cyanamide, We had previously shown that in unbuffered aqueous solution, cyanoacetylene, glycolaldehyde, glyceraldehyde and inorganic 2-amino-oxazole 11 adds to glyceraldehyde 9 to give the pentose phosphate—are plausible prebiotic feedstock molecules12–15, and amino-oxazolines including 12 in excellent overall yield20. Our start- the conditions of the synthesis are consistent with potential ing point in the present work was therefore to find a prebiotically early-Earth geochemical models. Although inorganic phosphate is only incorporated into the nucleotides at a late stage of the O O OH sequence, its presence from the start is essential as it controls three 10 OH HO OH reactions in the earlier stages by acting as a general acid/base cata- HO O lyst, a nucleophilic catalyst, a pH buffer and a chemical buffer. For OH 4 (p) prebiotic reaction sequences, our results highlight the importance 9 OH N HO of working with mixed chemical systems in which reactants for a NH H2N CN 2 O –H O OH particular reaction step can also control other steps. 8 2 O 11 HO Because they comprise phosphate, ribose and nucleobases, it is +H O 2 O HO OH 4 (f) tempting to assume that ribonucleotides must have prebiotically N H N NH2 2 NH assembled from such building blocks. Thus, for example, it has previ- HO O 2 O 12 NH2 ously been supposed that the activated ribonucleotide b-ribocytidine- 6 N 29,39-cyclic phosphate 1 must have been produced by phosphorylation X –H O 2 N O of the ribonucleoside 2, with the latter deriving from the conjoining of H –H2O O 3 the free pyrimidine nucleobase cytosine 3 and the furanose form of CN 5 ribose 4 (Fig. 1, blue arrows). This mode of assembly is seemingly NH HO 2 supported by the facts that cytosine 3 can be synthesized by condensa- +H O O N N tion of cyanoacetaldehyde 5 and urea 616 (the hydration products of 2 cyanoacetylene 717, and cyanamide 818, respectively) and pentoses CN O 7 HO2 OH including ribose can be produced by aldol reaction of glyceraldehyde HO OH 8,9 P 9 and glycolaldehyde 10 . The insuperable problem with this –2H2O O O– NH2 approach, however, is that one of the presumed steps, the condensa- Pi HO 11 HO O tion of ribose 4 and cytosine 3, does not work . The reasons for this are O N N N + both kinetic (the N1 lone pair of 3 is unavailable owing to delocaliza- O NH2 –H2O O N O O tion) and, in water, thermodynamic (the equilibrium constant is such HO 13 P thathydrolysis of2 to 3 and4 isfavouredovercondensation).The same OO– 1 is true for ribosylation of uracil, which has also not been demonstrated. Figure 1 | Pyrimidine ribonucleotide assembly options. Previously assumed We have considered a large number of alternative ribonucleotide synthesis of b-ribocytidine-29,39-cyclic phosphate 1 (blue; note the failure of assembly modes, including those that extend back to the same small- the step in which cytosine 3 and ribose 4 are proposed to condense together) molecule precursors as the traditionally assumed route described and the successful new synthesis described here (green). p, pyranose; f, above19. By systematic experimental investigation of these options, furanose. 1School of Chemistry, The University of Manchester, Oxford Road, Manchester M13 9PL, UK. 239 ©2009 Macmillan Publishers Limited. All rights reserved LETTERS NATURE | Vol 459 | 14 May 2009 plausible synthesis of 11. Constitutionally, 11 is the condensation We then investigated whether the subsequent reaction of 11 with product of 8 and 10, and although there exists, in the conventional glyceraldehyde 9 would be tolerant to the residual presence of phos- chemical literature, a procedure to bring about this condensation, it phate. In the absence of phosphate, the ribose and arabinose amino- requires strongly alkaline conditions21. Because we wanted to oxazolines 21 and 12 are the major products, and the xylose derivative generate 11, and then allow it to react with 9, which is unstable to 22 is a minor product (Fig. 3a)20. The lyxose amino-oxazoline 23 is alkali, under the same conditions, neutral-pH reaction conditions formed in intermediate amounts as an equilibrating mixture of had to be found. pyranose and furanose isomers. All of the pentose amino-oxazolines We initially investigated the reaction with 8 and 10 in a 1:1 ratio have the potential to be converted reversibly into one or other of the starting at neutral pH in unbuffered aqueous solution. Only a small 5-substituted 2-amino-oxazoles 24 and 25 by phosphate catalysis (by amount of 11 was produced under these conditions, and 1H NMR chemistry similar to that underlying the conversion of 16 to 11), but to spectra were indicative of the formation of a variety of carbonyl addi- differing extents depending on their stability. After one day in the tion adducts and other intermediates, for example 14–18 (Fig. 2a, b). presence of phosphate, all of the amino-oxazolines showed some con- The carbonyl addition adducts 14 were presumably formed reversibly, version to the corresponding 5-substituted 2-amino-oxazole (24 or and so did not represent material irretrievably committed to other 25), but the lyxose amino-oxazoline 23 proved the least stable and products, but rather intermediates stalled en route to 11. At low con- underwent the greatest conversion (Fig. 3b). We then took a crude centrations of hydroxide, it appeared that two additional types of sample of 11 that had just been prepared from cyanamide 8 and reaction needed to make 11 were very sluggish: intra-adduct attack glycolaldehyde 10 in the presence of phosphate, and added glyceralde- of the glycolaldehyde-derived hydroxyl group on the cyanamide- hyde 9 to it. After overnight incubation, 1H NMR analysis revealed that derived nitrile carbon (for example 14 (n 5 0) R 15), and C–H depro- although all four amino-oxazolines were still formed, the lyxose deri- tonation leading to aromatization (17 R 11). vative 23 was selectively depleted and was now a minor product along Denied the opportunity of using hydroxide as a specific base cata- with the xylose derivative 22 (Fig. 3c). With two of its stereoisomeric lyst to accelerate these slow steps, we sought a general base catalyst that relatives now minor products, the path from the arabinose amino- could provide the same acceleration, but at neutral pH. Inorganic oxazoline 12 to ribonucleotides looked clearer. Selective crystallization phosphate seemed to be ideal in this regard because its second pKa of ribose amino-oxazoline 21 offers a further means of enriching 12 value is close to neutrality. Furthermore, as phosphate is ultimately such that it becomes the major product in solution20,22. needed in some form to make activated nucleotides, we decided to We then proceeded to the second stage of pyrimidine nucleobase include it from the start of the assembly sequence. We repeated the assembly. Although our focus was on the chemistry of the key arabinose earlier reaction of cyanamide 8 and glycolaldehyde 10, but in the amino-oxazoline 12, the corresponding chemistry of the ribose amino- presence of 1 M phosphate buffer at pH 7.0. 1H NMR analysis revealed oxazoline 21 was also studied (Supplementary Information). It had that 2-amino-oxazole 11 was produced in .80% yield (75% isolated earlier been shown that in unbuffered aqueous solution, 12 reacts with yield) (Fig. 2c). With an excess of 8 over 10, the synthesis of 11 still an excess of cyanoacetylene 7 giving b-arabinocytidine 26,(Fig.4a)23. takes place in the presence of phosphate, but is followed by slower The yield of 26 was relatively low, however, and we used 1HNMR phosphate addition to residual 8 giving the intermediate adduct 19, analysis to determine why.
Recommended publications
  • Interferometric Observations of Large Biologically Interesting Interstellar and Cometary Molecules
    SPECIAL FEATURE: PERSPECTIVE Interferometric observations of large biologically interesting interstellar and cometary molecules Lewis E. Snyder* Department of Astronomy, University of Illinois, 1002 West Green Street, Urbana, IL 61801 Edited by William Klemperer, Harvard University, Cambridge, MA, and approved May 26, 2006 (received for review March 3, 2006) Interferometric observations of high-mass regions in interstellar molecular clouds have revealed hot molecular cores that have sub- stantial column densities of large, partly hydrogen-saturated molecules. Many of these molecules are of interest to biology and thus are labeled ‘‘biomolecules.’’ Because the clouds containing these molecules provide the material for star formation, they may provide insight into presolar nebular chemistry, and the biomolecules may provide information about the potential of the associated inter- stellar chemistry for seeding newly formed planets with prebiotic organic chemistry. In this overview, events are outlined that led to the current interferometric array observations. Clues that connect this interstellar hot core chemistry to the solar system can be found in the cometary detection of methyl formate and the interferometric maps of cometary methanol. Major obstacles to under- standing hot core chemistry remain because chemical models are not well developed and interferometric observations have not been very sensitive. Differentiation in the molecular isomers glycolaldehdye, methyl formate, and acetic acid has been observed, but not explained. The extended source structure for certain sugars, aldehydes, and alcohols may require nonthermal formation mechanisms such as shock heating of grains. Major advances in understanding the formation chemistry of hot core species can come from obser- vations with the next generation of sensitive, high-resolution arrays.
    [Show full text]
  • 'Impossible' Cloud on Titan Explained
    ‘Impossible’ Cloud on Titan Explained Cloud crystals in the super-cold environment of Titan are revealing surprising solid-state chemical processes that illuminate similar chemistry occurring in Earth’s polar stratospheric clouds. Titan’s spring brings polar ice clouds made of dicyanoacetylene (C4N2) molecules. The presence of these polar clouds seemed impossible, because Cassini infrared measurements showed there is not enough C4N2 in the stratosphere to form the observed ice clouds. So where does the C4N2 come from? Cassini found that springtime sunshine kicks off an ‘on-site’ manufacturing process that produces the icy raw material for the C4N2 clouds. Photochemical reactions between hydrogen cyanide (HCN) and cyanoacetylene (HC3N) in Titan’s stratosphere were found to produce C4N2 .This unexpected photochemical effect on icy solids explains how these Titan’s Icy Polar Clouds The cloud at right seemingly ‘impossible’ clouds form in Titan’s springtime polar contains HCN. Some stratosphere! other polar stratospheric clouds are made of Something similar occurs in Earth’s polar stratosphere, where dicyanoacetylene (C4N2) which is produced from solid-state chemistry involving chlorine is at the heart of ozone sunlight-driven processes loss in Earth’s atmosphere. Comparison of the atmospheres of occurring on frozen Earth and Titan informs us on the fundamental processes that organic particles. A similar process is seen in occur throughout nature. Earth’s stratosphere between gases and water Solid-state photochemistry as a formation mechanism for Titan's stratospheric ice particles. C4N2 ice clouds. C. Anderson, R. Samuelson, Y. Yung and J. McLain, Geophysical Research Letters, 43, 3088-3094, 2016. .
    [Show full text]
  • Life As a Guide to Prebiotic Nucleotide Synthesis
    COMMENT DOI: 10.1038/s41467-018-07220-y OPEN Life as a guide to prebiotic nucleotide synthesis Stuart A. Harrison1 & Nick Lane 1 Synthesis of activated nucleotides has been accomplished under ‘prebiotically plausible’ conditions, but bears little resemblance to the chemistry of life as we know it. Here we argue that life is an indispensable guide to its own origins. 1234567890():,; “The justification of prebiotic syntheses by appealing to their similarity to enzymatic mechanisms has been routine in the literature of prebiotic chemistry. Acceptance of the RNA World hypothesis invalidates this type of argument. If the RNA World originated de novo on the primitive Earth, it erects an almost opaque barrier between biochemistry and prebiotic chemistry.” Leslie Orgel 2004. There is little doubt that RNA is central to the origins of genetic information and protein synthesis, but that is a far cry from the stronger statement, articulated by Orgel, that if metabolism arose from an RNA world, then life can give no insights into its own origin1. Yet this view resonates with much prebiotic chemistry over the last decade. Activated pyrimidine and oxopurine nucleotides have been synthesised at good yield from purportedly prebiotically plausible precursors such as cyanide and cyanoacetylene, driven by UV radiation2. Wet-dry cycles in the presence of laminated clay minerals and lipids can polymerise nucleotides to RNA3. Accordingly, some claim that the problem has already been solved, at least conceptually. Has it? Not in everybody’s view. Perhaps the biggest problem is that the chemistry involved in these clever syntheses does not narrow the gap between prebiotic chemistry and biochemistry—it does not resemble extant biochemistry in terms of substrates, reaction pathways, catalysts or energy coupling4.
    [Show full text]
  • The Dissipative Photochemical Origin of Life: UVC Abiogenesis of Adenine
    entropy Article The Dissipative Photochemical Origin of Life: UVC Abiogenesis of Adenine Karo Michaelian Department of Nuclear Physics and Applications of Radiation, Instituto de Física, Universidad Nacional Autónoma de México, Circuito Interior de la Investigación Científica, Cuidad Universitaria, Mexico City, C.P. 04510, Mexico; karo@fisica.unam.mx Abstract: The non-equilibrium thermodynamics and the photochemical reaction mechanisms are described which may have been involved in the dissipative structuring, proliferation and complex- ation of the fundamental molecules of life from simpler and more common precursors under the UVC photon flux prevalent at the Earth’s surface at the origin of life. Dissipative structuring of the fundamental molecules is evidenced by their strong and broad wavelength absorption bands in the UVC and rapid radiationless deexcitation. Proliferation arises from the auto- and cross-catalytic nature of the intermediate products. Inherent non-linearity gives rise to numerous stationary states permitting the system to evolve, on amplification of a fluctuation, towards concentration profiles providing generally greater photon dissipation through a thermodynamic selection of dissipative efficacy. An example is given of photochemical dissipative abiogenesis of adenine from the precursor HCN in water solvent within a fatty acid vesicle floating on a hot ocean surface and driven far from equilibrium by the incident UVC light. The kinetic equations for the photochemical reactions with diffusion are resolved under different environmental conditions and the results analyzed within the framework of non-linear Classical Irreversible Thermodynamic theory. Keywords: origin of life; dissipative structuring; prebiotic chemistry; abiogenesis; adenine; organic molecules; non-equilibrium thermodynamics; photochemical reactions Citation: Michaelian, K. The Dissipative Photochemical Origin of MSC: 92-10; 92C05; 92C15; 92C40; 92C45; 80Axx; 82Cxx Life: UVC Abiogenesis of Adenine.
    [Show full text]
  • Pyrolysis and Combustion of Acetonitrile (Ch3cn)
    OAK RIDGE ORNL/TM-2002/113 NATIONAL LABORATORY MANAGED BY UT-BATTELLE FOR THE DEPARTMENT OF ENERGY Pyrolysis and Combustion of Acetonitrile (CH3CN) Phillip F. Britt DOCUMENT AVAILABILITY Reports produced after January 1, 1996, are generally available free via the U.S. Department of Energy (DOE) Information Bridge. Web site http://www.osti.gov/bridge Reports produced before January 1, 1996, may be purchased by members of the public from the following source. National Technical Information Service 5285 Port Royal Road Springfield, VA 22161 Telephone 703-605-6000 (1-800-553-6847) TDD 703-487-4639 Fax 703-605-6900 E-mail [email protected] Web site http://www.ntis.gov/support/ordernowabout.htm Reports are available to DOE employees, DOE contractors, Energy Technology Data Exchange (ETDE) representatives, and International Nuclear Information System (INIS) representatives from the following source. Office of Scientific and Technical Information P.O. Box 62 Oak Ridge, TN 37831 Telephone 865-576-8401 Fax 865-576-5728 E-mail [email protected] Web site http://www.osti.gov/contact.html This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof.
    [Show full text]
  • Investigating the Chemical Composition of the CIRS-Observed 160 Cm-1 Ice Cloud in Titan’S Stratosphere
    EPSC Abstracts Vol. 14, EPSC2020-423, 2020 https://doi.org/10.5194/epsc2020-423 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Investigating the Chemical Composition of the CIRS-Observed 160 cm-1 Ice Cloud in Titan’s Stratosphere Melissa Ugelow1,2 and Carrie Anderson1 1NASA Goddard Space Flight Center, Astrochemistry Laboratory, Greenbelt, MD, United States of America 2Universities Space Research Association, Columbia, MD, United States of America Remote sensing observations from Voyager 1’s InfraRed Interferometer Spectrometer (IRIS) and Cassini’s Composite InfraRed Spectrometer (CIRS) confirmed the presence of nitrile ice clouds in Titan’s stratosphere (Samuelson 1985, 1992; Khanna, R.K. et al., 1987; Samuelson et al., 1997, 2007; Coustenis, A. et al., 1999; Mayo and Samuelson, 2005; Anderson, C.M. et al., 2010, 2018a,b; Anderson and Samuelson, 2011). While individual gases in Titan’s stratosphere are expected to condense to form pure ices, some of these gases will enter altitude regions where they undergo simultaneous saturation, or co-condensation, and form a mixed ice. The infrared spectral features resulting from a mixed ice have their own unique spectral signatures that notably diverge from the weighted sum of the individual species, and must therefore be experimentally determined as functions of temperature and mixing ratio (Anderson and Samuelson, 2011; Anderson et al. 2018a,b). The first observation of a co-condensate in Titan’s stratosphere was acquired by CIRS, which revealed a spectrally broad quasi-continuum ice emission feature with a spectral peak near 160 cm-1.
    [Show full text]
  • Soups & SELEX for the Origin of Life
    Downloaded from rnajournal.cshlp.org on September 25, 2021 - Published by Cold Spring Harbor Laboratory Press Soups & SELEX for the origin of life RENÉE SCHROEDER Max F. Perutz Laboratories, University of Vienna, 1030 Vienna, Austria The theory of evolution quickly brought up the most fasci- grounds on which chemists could develop experimental nating question in biology: the origin of life. How did life set ups. Combinatorial events of simple chemical reactions emerge? The biggest challenge in this endeavor to understand could lead to stably replicating populations of increasing how life could have emerged without a controller is to unravel complexity. the chemical processes that made the synthesis of complex molecules containing information possible. Primordial Soups: prebiotic chemistry needs Already at high school I was totally caught by Oparin’s hy- to deliver activated ribonucleotides pothesis that simple unicellular organisms evolved from sim- ple organic molecules, which in turn originated from simple One prerequisite for the emergence of Life is the condensa- inorganic molecules present in the early atmosphere of our tion of informational polymers by purely chemical means. planet. Oparin and Haldane coined the idea of “primordial Indeed, the Orgel lab has been successful in obtaining nucle- soup” experiments. For my “Matura” (that is the name of otide polymers as long as 55 monomers in the presence of the exam you do in Austria, when you finally leave high mineral surfaces like montmorillonite. For this to happen school) I got Stanley Miller’s famous primordial soup exper- activated ribonucleotide building blocks must have been iments as question. I just now realize that ever since SOUP & available in sufficient amounts.
    [Show full text]
  • Photodissociation Dynamics in Titan's Atmosphere Welvidanalage Ruchira Silva Wayne State University
    Wayne State University DigitalCommons@WayneState Wayne State University Dissertations 1-1-2010 Photodissociation Dynamics In Titan's Atmosphere Welvidanalage Ruchira Silva Wayne State University Follow this and additional works at: http://digitalcommons.wayne.edu/oa_dissertations Recommended Citation Silva, Welvidanalage Ruchira, "Photodissociation Dynamics In Titan's Atmosphere" (2010). Wayne State University Dissertations. Paper 63. This Open Access Dissertation is brought to you for free and open access by DigitalCommons@WayneState. It has been accepted for inclusion in Wayne State University Dissertations by an authorized administrator of DigitalCommons@WayneState. PHOTODISSOCIATION DYNAMICS IN TITAN’S ATMOSPHERE by W. RUCHIRA SILVA DISSERTATION Submitted to the Graduate School of Wayne State University, Detroit, Michigan in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY 2010 MAJOR: CHEMISTRY (Physical) Approved by: Advisor Date © COPYRIGHT BY WELVIDANALAGE RUCHIRA ROHAN SILVA 2010 All Rights Reserved DEDICATION ~ To my Parents, Madu and Netuli… ii ACKNOWLEDGMENTS First and foremost, I owe my deepest gratitude to my advisor, Professor Arthur G. Suits, whose guidance, encouragement and support enabled me to complete my graduate studies through Wayne State University. This dissertation would not have been possible without his forgiveness, kind considerations, great efforts and continuous support. I am very fortunate to have an advisor like Prof. Suits who not only guided me to understand the subject but also helped me to overcome every major difficulty I faced in my life over the last five years. If it was not his support my dreams would not have become a reality. His passion towards research is inspiring and motivating. I’m grateful for him for everything I learnt throughout my graduate career.
    [Show full text]
  • United States Patent Office 3,979,424
    United States Patent Office Fazented Feb.3,979,424 26, 1963 2 Table I 3,079,424 Pike CESS FOR THE REPARATSN OF CYAN. Yield (perceit based on ACETYSLENE FRCS ACETYLENE AND HYDER- R T Moe rati E. HCN) GEN CYANOE a- SP SEO E------ Eawrence J. Krebaum, Texas City, Tex., assignor to No. C. CN:CH: A ES Cyano- Acrylo- (CN) Measante Chenaica Company, St. Louis, Mo., a corpo- acetylene nitrile ration of Delaware No. 33awing. Fied Oct. 24, 1960, Ser. No. 64,290 70 4:3, 5 : 0.36 4.3 38. 6 3 (Caimas. (C. 260-455.3) 85 4:1:7 0.38 3.6 3.2 6. The present invention relates to a new method for the 5.3: E. 5.5:5515:19: 835.3 33.6g 33.6: is 37 preparation of cyanoacetylene or propargyl nitrile. III SS 08: 83 : 3: 23 Cyanoacetylene, a chemical compound useful as a cyan ovinylating agent in the production of cyanovinyl mono mers, has heretofore been obtained from propiolic acid 15 It will be seen from the tabulated data that not only by converting the acid to the corresponding amide and is cyanoacetylene formed in good yields but acrylonitrile, then dehydrating the latter with phosphorus penioxide. a valuable chemical of commerce, is also produced as is It has now been discovered that this interesting and re- cyanogen. In view of the fact that it has recently been active compound can be prepared in a relatively simple determined that cyanogen will react with acetylene under manner directly from acetylene.
    [Show full text]
  • Organic Synthesis Applied to Space Sciences J.-C
    EPJ Web of Conferences 18, 06004 (2011) DOI: 10.1051/epjconf/20111806004 C Owned by the authors, published by EDP Sciences, 2011 Organic synthesis applied to space sciences J.-C. Guillemina École Nationale Supérieure de Chimie de Rennes, CNRS, UMR 6226, Avenue du Général Leclerc, CS 50837, 35708 Rennes Cedex 7, France Abstract. About 160 molecules have been detected in the interstellar medium, the comae and the atmospheres of planets. The presence of these compounds leads to imagine a chemistry of these media to explain the formation of these species and to predict the possible presence of other ones. Many of them have never been synthesized or isolated in labs and their preparation can be challenging, up to necessitate news reactions or special equipments. INTRODUCTION The recording of the Infrared (IR), Ultraviolet (UV) and Microwave (MW) spectra of many places of the Universe shows signals corresponding to complex mixtures of molecules. The identification of about 150 molecules in the interstellar medium (ISM) [1], of dozens in comae and in the planetary atmospheres (Jupiter, Saturn, Neptune, Venus, Titan (the largest moon of Saturn), ...)hasgenerated many attempts to know how they are formed and eventually decomposed, and to predict which other compounds could be observed in these media. The understanding of the chemistry of the ISM, of planetary atmospheres including the Earth is probably one of the most intriguing research subjects. For a long time, the region between the stars was considered to be too hostile to contain quantities of molecules, but at the end of the 1960s, ammonia [2], water [3, 4] and formaldehyde [5] were observed.
    [Show full text]
  • Ionization Photophysics and Spectroscopy of Cyanoacetylene Sydney Leach, Gustavo A
    Ionization photophysics and spectroscopy of cyanoacetylene Sydney Leach, Gustavo A. Garcia, Ahmed Mahjoub, Yves Bénilan, Nicolas Fray, Marie-Claire Gazeau, François Gaie-Levrel, Norbert Champion, and Martin Schwell Citation: The Journal of Chemical Physics 140, 174305 (2014); doi: 10.1063/1.4871298 View online: http://dx.doi.org/10.1063/1.4871298 View Table of Contents: http://scitation.aip.org/content/aip/journal/jcp/140/17?ver=pdfcov Published by the AIP Publishing Articles you may be interested in Ionization photophysics and spectroscopy of dicyanoacetylene J. Chem. Phys. 139, 184304 (2013); 10.1063/1.4826467 A femtosecond velocity map imaging study on B-band predissociation in CH3I. II. The 2 0 1 and 3 0 1 vibronic levels J. Chem. Phys. 136, 074303 (2012); 10.1063/1.3683252 Resonantly enhanced multiphoton ionization and zero kinetic energy photoelectron spectroscopy of 2-indanol conformers J. Chem. Phys. 124, 204306 (2006); 10.1063/1.2201747 Resonantly enhanced two photon ionization and zero kinetic energy spectroscopy of jet-cooled 4-aminopyridine J. Chem. Phys. 120, 7497 (2004); 10.1063/1.1687673 Multiphoton ionization and photoelectron spectroscopy of formaldehyde via its 3p Rydberg states J. Chem. Phys. 114, 9797 (2001); 10.1063/1.1370943 This article is copyrighted as indicated in the article. Reuse of AIP content is subject to the terms at: http://scitation.aip.org/termsconditions. Downloaded to IP: 193.51.99.1 On: Fri, 20 Jun 2014 12:55:42 THE JOURNAL OF CHEMICAL PHYSICS 140, 174305 (2014) Ionization photophysics and spectroscopy of cyanoacetylene Sydney Leach,1,a) Gustavo A. Garcia,2 Ahmed Mahjoub,3 Yves Bénilan,3 Nicolas Fray,2 Marie-Claire Gazeau,3 François Gaie-Levrel,2,b) Norbert Champion,1 and Martin Schwell3,a) 1LERMA UMR CNRS 8112, Observatoire de Paris-Meudon, 5 place Jules-Jansen, 92195 Meudon, France 2Synchrotron SOLEIL, L’Orme des Merisiers, St.
    [Show full text]
  • Irradiation of Mixtures of Gases That Simulate Titan's Atmosphere
    Icarus 177 (2005) 106–115 www.elsevier.com/locate/icarus Photochemical processes on Titan: Irradiation of mixtures of gases that simulate Titan’s atmosphere Buu N. Tran a,JeffreyC.Josepha, Michael Force b, Robert G. Briggs b, Veronique Vuitton a, JamesP.Ferrisa,∗ a Department of Chemistry, Rensselaer Polytechnic Institute, Troy, NY 12180-3590, USA b Wadsworth Center for Laboratories and Research, NY State Department of Health, Albany, NY 12201, USA Received 3 November 2004; revised 14 January 2005 Available online 17 May 2005 Abstract Photochemical reaction pathways in Titan’s atmosphere were investigated by irradiation of the individual components and the mixture containing nitrogen, methane, hydrogen, acetylene, ethylene, and cyanoacetylene. The quantum yields for the loss of the reactants and the formation of products were determined. Photolysis of ethylene yields mainly saturated compounds (ethane, propane, and butane) while photolysis of acetylene yields the same saturated compounds as well as ethylene and diacetylene. Irradiation of cyanoacetylene yields mainly hydrogen cyanide and small amounts of acetonitrile. When an amount of methane corresponding to its mixing ratio on Titan was added to these mixtures the quantum yields for the loss of reactants decreased and the quantum yields for hydrocarbon formation increased indicative of a hydrogen atom abstraction from methane by the photochemically generated radicals. GC/MS analysis of the products formed by irradiation of mixtures of all these gases generated over 120 compounds which were mainly aliphatic hydrocarbons containing double and triple bonds along with much smaller amounts of aromatic compounds like benzene, toluene and phenylacetylene. The reaction pathways were investigated by the use of 13C acetylene in these gas mixtures.
    [Show full text]