With Acetylene (C2H2;Xrg) ⇑ Tao Yang, Beni B
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Summary Tables of Calculated and Experimental Parameters Of
Summary Tables of Calculated and Experimental Parameters of Diatomic, Triatomic, Organic, Silicon, Boron, Aluminum and Organometallic Molecules, Exemplary Results on Condensed Matter Physics, One-Through Twenty-Electron Atoms, Excited States of Helium, g Factor, and Fundamental Particle Masses The closed-form derivations from Maxwell's equations given in The Grand Unified Theory of Classical Physics posted at http://www.blacklightpower.com/theory/bookdownload.shtml contain fundamental constants only. The nature of the chemical bond is given in Chapters 12 through 15. The atoms are solved exactly in Chapters 1, 7, and 10. The excited states of helium are solved exactly in Chapter 9. The electron g factor and relations between fundamental particles are given in Chapter 1 and Chapters 36, 37 and 38. Tables summarizing the results of the calculated experimental parameters of 800 exemplary solved molecules follow. The closed-form derivations of these molecules can be found in The Grand Theory of Classical Physics posted at http://www.blacklightpower.com/theory/bookdownload.shtml Chapters 15–17, as well as Silicon in Chapter 20, Boron in Chapter 22, and Aluminum and Organometallics in Chapter 23. Condensed matter physics based on first principles with analytical solutions of (i) of the geometrical parameters and energies of the hydrogen bond of H2O in the ice and steam phases, and of H2O and NH3; (ii) analytical solutions of the geometrical parameters and interplane van der Waals cohesive energy of graphite; (iii) analytical solutions of the geometrical parameters and interatomic van der Waals cohesive energy of liquid helium and solid neon, argon, krypton, and xenon are given in Chapter 16. -
The Observed Chemical Structure of L1544? ?? S
Astronomy & Astrophysics manuscript no. Maps_L1544 c ESO 2017 July 20, 2017 The observed chemical structure of L1544? ?? S. Spezzano, P. Caselli, L. Bizzocchi, B. M. Giuliano, and V. Lattanzi Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748 Garching, Germany July 20, 2017 ABSTRACT Context. Prior to star formation, pre-stellar cores accumulate matter towards the centre. As a consequence, their central density increases while the temperature decreases. Understanding the evolution of the chemistry and physics in this early phase is crucial to study the processes governing the formation of a star. Aims. We aim at studying the chemical differentiation of a prototypical pre-stellar core, L1544, by detailed molecular maps. In contrast with single pointing observations, we performed a deep study on the dependencies of chemistry on physical and external conditions. Methods. We present the emission maps of 39 different molecular transitions belonging to 22 different molecules in the central 6.25 arcmin2 of L1544. We classified our sample in five families, depending on the location of their emission peaks within the core. Furthermore, to systematically study the correlations among different molecules, we have performed the principal component analysis (PCA) on the integrated emission maps. The PCA allows us to reduce the amount of variables in our dataset. Finally, we compare the maps of the first three principal components with the H2 column density map, and the Tdust map of the core. Results. The results of our qualitative analysis is the classification of the molecules in our dataset in the following groups: (i) the c-C3H2 family (carbon chain molecules like C3H and CCS), (ii) the dust peak family (nitrogen-bearing species + like N2H ), (iii) the methanol peak family (oxygen-bearing molecules like methanol, SO and SO2), (iv) the HNCO peak family (HNCO, propyne and its deuterated isotopologues). -
Exhaustive Product Analysis of Three Benzene Discharges by Microwave Spectroscopy Michael C
pubs.acs.org/JPCA Article Exhaustive Product Analysis of Three Benzene Discharges by Microwave Spectroscopy Michael C. McCarthy,* Kin Long Kelvin Lee, P. Brandon Carroll, Jessica P. Porterfield, P. Bryan Changala, James H. Thorpe, and John F. Stanton Cite This: J. Phys. Chem. A 2020, 124, 5170−5181 Read Online ACCESS Metrics & More Article Recommendations *sı Supporting Information ABSTRACT: Using chirped and cavity microwave spectroscopies, automated double resonance, new high-speed fitting and deep learning algorithms, and large databases of computed structures, the discharge products of benzene alone, or in combination with molecular oxygen or nitrogen, have been exhaustively characterized between 6.5 and 26 GHz. In total, more than 3300 spectral features were observed; 89% of these, accounting for 97% of the total intensity, have now been assigned to 152 distinct chemical species and 60 of their variants (i.e., isotopic species and vibrationally excited states). Roughly 50 of the products are entirely new or poorly characterized at high resolution, including many heavier by mass than the precursor benzene. These findings provide direct evidence for a rich architecture of two- and three-dimensional carbon and indicate that benzene growth, particularly the formation of ring−chain molecules, occurs facilely under our experimental conditions. The present analysis also illustrates the utility of microwave spectroscopy as a precision tool for complex mixture analysis, irrespective of whether the rotational spectrum of a product species is known a priori or not. From this large quantity of data, for example, it is possible to determine with confidence the relative abundances of different product masses, but more importantly the relative abundances of different isomers with the same mass. -
A Chemical Kinetics Network for Lightning and Life in Planetary Atmospheres P
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by St Andrews Research Repository The Astrophysical Journal Supplement Series, 224:9 (33pp), 2016 May doi:10.3847/0067-0049/224/1/9 © 2016. The American Astronomical Society. All rights reserved. A CHEMICAL KINETICS NETWORK FOR LIGHTNING AND LIFE IN PLANETARY ATMOSPHERES P. B. Rimmer and Ch Helling School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK; [email protected] Received 2015 June 3; accepted 2015 October 22; published 2016 May 23 ABSTRACT There are many open questions about prebiotic chemistry in both planetary and exoplanetary environments. The increasing number of known exoplanets and other ultra-cool, substellar objects has propelled the desire to detect life andprebiotic chemistry outside the solar system. We present an ion–neutral chemical network constructed from scratch, STAND2015, that treats hydrogen, nitrogen, carbon, and oxygen chemistry accurately within a temperature range between 100 and 30,000 K. Formation pathways for glycine and other organic molecules are included. The network is complete up to H6C2N2O3. STAND2015 is successfully tested against atmospheric chemistry models for HD 209458b, Jupiter, and the present-day Earth using a simple one- dimensionalphotochemistry/diffusion code. Our results for the early Earth agree with those of Kasting for CO2,H2, CO, and O2, but do not agree for water and atomic oxygen. We use the network to simulate an experiment where varied chemical initial conditions are irradiated by UV light. The result from our simulation is that more glycine is produced when more ammonia and methane is present. -
Directed Gas Phase Formation of Silicon Dioxide and Implications for the Formation of Interstellar Silicates
ARTICLE DOI: 10.1038/s41467-018-03172-5 OPEN Directed gas phase formation of silicon dioxide and implications for the formation of interstellar silicates Tao Yang 1,2, Aaron M. Thomas1, Beni B. Dangi1,3, Ralf I. Kaiser 1, Alexander M. Mebel 4 & Tom J. Millar 5 1234567890():,; Interstellar silicates play a key role in star formation and in the origin of solar systems, but their synthetic routes have remained largely elusive so far. Here we demonstrate in a combined crossed molecular beam and computational study that silicon dioxide (SiO2) along with silicon monoxide (SiO) can be synthesized via the reaction of the silylidyne radical (SiH) with molecular oxygen (O2) under single collision conditions. This mechanism may provide a low-temperature path—in addition to high-temperature routes to silicon oxides in circum- stellar envelopes—possibly enabling the formation and growth of silicates in the interstellar medium necessary to offset the fast silicate destruction. 1 Department of Chemistry, University of Hawai’iatMānoa, Honolulu, HI 96822, USA. 2 State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai, 200062, China. 3 Department of Chemistry, Florida Agricultural and Mechanical University, Tallahassee, FL 32307, USA. 4 Department of Chemistry and Biochemistry, Florida International University, Miami, FL 33199, USA. 5 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN, UK. Correspondence and requests for materials should be addressed to R.I.K. (email: [email protected]) or to A.M.M. (email: mebela@fiu.edu) or to T.J.M. (email: [email protected]) NATURE COMMUNICATIONS | (2018) 9:774 | DOI: 10.1038/s41467-018-03172-5 | www.nature.com/naturecommunications 1 ARTICLE NATURE COMMUNICATIONS | DOI: 10.1038/s41467-018-03172-5 — 28 + 28 + he origin of interstellar silicate grains nanoparticles ( SiO2 ), and 44 ( SiO ). -
Gas Phase Formation of C-Sic3 Molecules in the Circumstellar Envelope of Carbon Stars
Gas phase formation of c-SiC3 molecules in the circumstellar envelope of carbon stars Tao Yanga,b,1,2, Luke Bertelsc,1, Beni B. Dangib,3, Xiaohu Lid,e, Martin Head-Gordonc,2, and Ralf I. Kaiserb,2 aState Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200062, P. R. China; bDepartment of Chemistry, University of Hawai‘iatManoa, Honolulu, HI 96822; cDepartment of Chemistry, University of California, Berkeley, CA 94720; dXinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, P. R. China; and eNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China Contributed by Martin Head-Gordon, May 17, 2019 (sent for review July 20, 2018; reviewed by Piergiorgio Casavecchia and David Clary) Complex organosilicon molecules are ubiquitous in the circumstel- Modern astrochemical models propose that the very first lar envelope of the asymptotic giant branch (AGB) star IRC+10216, silicon–carbon bonds are formed in the inner envelope of the but their formation mechanisms have remained largely elusive until carbon star, which is undergoing mass loss at the rates of several − now. These processes are of fundamental importance in initiating a 10 5 solar masses per year (22, 23). Pulsations from the central chain of chemical reactions leading eventually to the formation of star may initiate shocks, which (photo)fragment the circumstellar — organosilicon molecules among them key precursors to silicon car- materials (24, 25). These nonequilibrium conditions cause tem- — bide grains in the circumstellar shell contributing critically to the peratures of 3,500 K or above (19) and lead to highly reactive galactic carbon and silicon budgets with up to 80% of the ejected metastable fragments such as electronically excited silicon atoms, materials infused into the interstellar medium. -
Most Common Substances in Chemicals for Different Industries
Table 14 Most common substances by industry Figures for 2009. Substances contained in more than 10 products. A substance can be omitted for secrecy reasons. Industry CAS-no Substance Number of products A01 Agriculture 7732-18-5 Water 458 6484-52-2 Nitric acid ammonium salt 77 57-55-6 1,2-Propanediol 75 64742-65-0 Distillates (petroleum), solvent-dewaxed heavy 74 paraffinic 63148-62-9 Siloxanes and Silicones, di-Me 60 57-13-6 Urea 54 67-63-0 2-Propanol 54 11138-66-2 Xanthan gum 53 7783-20-2 Sulfuric acid diammonium salt 53 7722-76-1 Phosphoric acid, monoammonium salt 52 7487-88-9 Sulfuric acid magnesium salt (1:1) 51 7447-40-7 Potassium chloride 46 56-81-5 1,2,3-Propanetriol 44 7778-80-5 Sulfuric acid dipotassium salt 43 1310-73-2 Sodium hydroxide 41 7647-14-5 Sodium chloride 41 2634-33-5 1,2-Benzisothiazol-3(2H)-one 38 1310-58-3 Potassium hydroxide 33 7757-79-1 Nitric acid potassium salt 33 7785-87-7 Manganese sulfate 32 7664-38-2 Phosphoric acid 32 72623-87-1 Lubricating oils, petroleum, C20-50, 31 hydrotreated neutral oil-based 64741-89-5 Distillates (petroleum), solvent-refined light 29 paraffinic 77-92-9 1,2,3-Propanetricarboxylic acid, 2-hydroxy- 28 8061-51-6 Lignosulfonic acid, sodium salt 28 7778-18-9 Sulfuric acid, calcium salt (1:1) 27 64-17-5 Ethanol 27 14807-96-6 Talc 26 64742-94-5 Solvent naphtha (petroleum), heavy arom. 25 68649-42-3 Phosphorodithioic acid, O,O-di-C1-14-alkyl 24 esters, zinc salts (2:1) 64-02-8 Glycine, N,N'-1,2-ethanediylbis[N- 24 (carboxymethyl)-, tetrasodium salt 64-19-7 Acetic acid 23 99-76-3 Benzoic acid, -
A Study of the C3H2 Isomers and Isotopologues: first Interstellar Detection of HDCCC?
A&A 586, A110 (2016) Astronomy DOI: 10.1051/0004-6361/201527460 & c ESO 2016 Astrophysics A study of the C3H2 isomers and isotopologues: first interstellar detection of HDCCC? S. Spezzano1;3, H. Gupta2;??, S. Brünken3, C. A. Gottlieb4, P. Caselli1, K. M. Menten5, H. S. P. Müller3, L. Bizzocchi1, P. Schilke3, M. C. McCarthy4, and S. Schlemmer3 1 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, 85748 Garching, Germany e-mail: [email protected] 2 California Institute of Technology, 770 S. Wilson Ave., M/C 100-22, Pasadena, CA 91125, USA 3 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany 4 Harvard-Smithsonian Center for Astrophysics, and School of Engineering & Applied Sciences, Harvard University, Cambridge, MA 02138, USA 5 Max-Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany Received 28 September 2015 / Accepted 12 November 2015 ABSTRACT The partially deuterated linear isomer HDCCC of the ubiquitous cyclic carbene (c-C3H2) was observed in the starless cores TMC- 1C and L1544 at 96.9 GHz, and a confirming line was observed in TMC-1 at 19.38 GHz. To aid the identification in these narrow line sources, four centimetre-wave rotational transitions (two in the previously reported Ka = 0 ladder and two new ones in the Ka = 1 ladder) and 23 transitions in the millimetre band between 96 and 272 GHz were measured in high-resolution laboratory spectra. Ten spectroscopic constants in a standard asymmetric top Hamiltonian allow the main transitions of astronomical interest −1 in the Ka ≤ 3 rotational ladders to be calculated to within 0.1 km s in radial velocity up to 400 GHz. -
Reaction Pathways Linking Chemisorption to Desorption of Methylchlorosilanes on Copper(001)
REACTION PATHWAYS LINKING CHEMISORPTION TO DESORPTION OF METHYLCHLOROSILANES ON COPPER(001) BY JAMES LALLO A dissertation submitted to the Graduate School|New Brunswick Rutgers, The State University of New Jersey in partial fulfillment of the requirements for the degree of Doctor of Philosophy Graduate Program in Chemistry and Chemical Biology Written under the direction of Professor B.J. Hinch and approved by New Brunswick, New Jersey October, 2012 ABSTRACT OF THE DISSERTATION Reaction pathways linking chemisorption to desorption of methylchlorosilanes on copper(001) by James Lallo Dissertation Director: Professor B.J. Hinch The interactions of silane molecules with metal surfaces are pivotal in many com- mercial processes. Of particular interest is the commercial \Direct Process," in which methyl chloride (CH3Cl) is exposed to silicon, in the presence of a copper catalyst and other promoters, producing dimethyldichlorosilane as the predominant product. Previous UHV studies have investigated the interaction of \pre-dissociated" methyl (CH3) and chlorine (Cl) with copper and copper-silicide surfaces. This thesis investi- gates the reaction mechanisms of \pre-associated" methylchlorosilanes ((CH3)xClySiHz, x+y+z=4) adsorbed on a copper(001) surface. The goal was to develop an understand- ing of the intermediates and transfer processes involved for dissociative adsorption and subsequent desorption of these molecules. Only molecules containing at least one Si- H bond were observed to undergo chemisorption. It was found that dimethylsilane (CH3)2SiH2 and methylsilane (CH3)SiH3 exhibit ligand transfer on the copper sur- face, leading to the desorption of trimethylsilane (CH3)3SiH, in both cases. The sug- gested intermediates present after adsorption of methylsilane were methylsilyl CH3SiH2, methysilylene CH3SiH and methylsilylidyne CH3Si. -
Gas Phase Synthesis of Interstellar Cumulenes. Mass Spectrometric and Theoretical Studies."
rl ì 6. .B,1l thesis titled: "Gas Phase Synthesis of Interstellar Cumulenes. Mass Spectrometric and Theoretical studies." submitted for the Degree of Doctor of Philosophy (Ph.D') by Stephen J. Blanksby B.Sc.(Hons,) from the Department of ChemistrY The University of Adelaide Cì UCE April 1999 Preface Contents Title page (i) Contents (ii) Abstract (v) Statement of OriginalitY (vi) Acknowledgments (vii) List of Figures (ix) Phase" I Chapter 1. "The Generation and Characterisation of Ions in the Gas 1.I Abstract I 1.II Generating ions 2 t0 l.ru The Mass SPectrometer t2 1.IV Characterisation of Ions 1.V Fragmentation Behaviour 22 Chapter 2 "Theoretical Methods for the Determination of Structure and 26 Energetics" 26 2,7 Abstract 27 2.IT Molecular Orbital Theory JJ 2.TII Density Functional Theory 2.rv Calculation of Molecular Properties 34 2.V Unimolecular Reactions 35 Chapter 3 "Interstellar and Circumstellar Cumulenes. Mass Spectrometric and 38 Related Studies" 3.I Abstract 38 3.II Interstellar Cumulenes 39 3.III Generation of Interstellar Cumulenes by Mass Spectrometry 46 3.IV Summary 59 Preface Chapter 4 "Generation of Two Isomers of C5H from the Corresponding Anions' 61 ATheoreticallyMotivatedMassSpectrometricStudy.'. 6l 4.r Abstract 62 4.rl Introduction 66 4.III Results and Discussion 83 4.IV Conclusions 84 4.V Experimental Section 89 4.VI Appendices 92 Chapter 5 "Gas Phase Syntheses of Three Isomeric CSHZ Radical Anions and Their Elusive Neutrals. A Joint Experimental and Theoretical Study." 92 5.I Abstract 93 5.II Introduction 95 5.ru Results and Discussion t12 5.IV Conclusions 113 5.V Experimental Section ttl 5.VI Appendices t20 Chapter 6 "Gas Phase Syntheses of Three Isomeric ClHz Radical Anions and Their Elusive Neutrals. -
On the Road to Carbene and Carbyne Complexes
ON THE ROAD TO CARBENE AND CARBYNE COMPLEXES Nobel Lecture, 11 December 1973 by ERNST OTTO FISCHER Inorganic Chemistry Laboratory, Technical University, Munich, Federal Republic of Germany Translation from the German text INTRODUCTION In the year 1960, I had the honour of giving a talk at this university* about sandwich complexes on which we were working at that time. I think I do not have to repeat the results of those investigations today. I would like to talk instead about a field of research in which we have been intensely interested in recent years: namely, the field of carbene complexes and, more recently, carbyne complexes. If we substitute one of the hydrogen atoms in a hydrocarbon of the alkane type - for example, ethane - by a metal atom, which can of course bind many more ligands, we arrive at an organometallic compound in which the organic radical is bound to the metal atom by a σ-bond (Fig. la). The earliest compounds of this kind were prepared more than a hundred years ago; the first was cacodyl, prepared by R. Bunsen (1), and then zinc dialkyls were prepared by E. Frankland (2). Later V. Grignard was able to synthesise alkyl magnesium halides by treating magnesium with alkyl halides (3). Grignard was awarded the Nobel Prize in 1912 for this effort. We may further recall the organo-aluminium compounds (4) of K. Ziegler which form the basis for the low pressure polymerisation, for example of ethylene. Ziegler and G. Natta were together honoured with the Nobel Prize in 1963 for their work on organometallic compounds. -
Transfer of Radiation Through Cyclopropenylidene and Ethylene Oxide
A&A 402, 1–3 (2003) Astronomy DOI: 10.1051/0004-6361:20030229 & c ESO 2003 Astrophysics Transfer of radiation through cyclopropenylidene and ethylene oxide S. Chandra School of Physical Sciences, SRTM University, Nanded 431 606, India Received 29 June 1999 / Accepted 17 October 2002 Abstract. Cyclopropenylidene and ethylene oxide molecules are of astronomical importance as their observed lines, distributed throughout the observable microwave region, have a number of pairs having nearly equal frequencies, but different excitation energies and/or belonging to two different species of the molecule. Hence, these molecules may play important role in detecting physical conditions in cosmic objects. Therefore, in order to calculate intensities of the lines, we have investigated transfer of radiation through a cosmic object containing the molecule at a kinetic temperature of 10 K. Our results show that some lines of the molecule may be found in absorption against the cosmic 2.7 K background. Key words. ISM: molecules – molecular data – radiative transfer 1. Introduction The molecular data required as input for the present inves- tigation are: (i) Einstein A-coefficients for radiative transitions Cyclopropenylidene (C3H2), in astronomical objects, was iden- between the rotational energy levels accounted for, and (ii) rate tified by Thaddeus et al. (1985); they reported twelve emission coefficients for collisional transitions between the energy levels lines of the molecule, distributed throughout the observable mi- due to collisions with H2 molecules. crowave region. Ethylene oxide (C H O) has been observed by 2 4 Both cyclopropenylidene and ethylene oxide are b-type Dickens et al. (1997) in Sgr B2N; twelve emission lines of the asymmetric top molecules having a large electric dipole mo- molecule, distributed throughout the observable microwave re- ment of 3.325 D and 1.88 D, respectively, along their b-axis gion, have been reported by them.