Bibliografías temáticas / Interstellar ices. carbon monoxide

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Literatura académica sobre el tema "Interstellar ices. carbon monoxide"

Autor: Grafiati
Publicado: 21 de diciembre de 2024
Última modificación: 31 de julio de 2025

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Artículos de revistas sobre el tema "Interstellar ices. carbon monoxide"

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Wang, Jia, Andrew M. Turner, Joshua H. Marks, et al. "Preparation of Acetylenediol (HOCCOH) and Glyoxal (HCOCHO) in Interstellar Analog Ices of Carbon Monoxide and Water." Astrophysical Journal 967, no. 2 (2024): 79. http://dx.doi.org/10.3847/1538-4357/ad3c3e.

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Abstract Enols—tautomers of ketones or aldehydes—are considered key intermediates in the formation of prebiotic sugars and sugar acids. Although laboratory simulation experiments suggest that enols should be ubiquitous in the interstellar medium, the underlying formation mechanisms of enols in interstellar environments are largely elusive. Here, we present the laboratory experiments on the formation of glyoxal (HCOCHO) along with its ynol tautomer acetylenediol (HOCCOH) in interstellar ice analogs composed of carbon monoxide (CO) and water (H2O) upon exposure to energetic electrons as a proxy
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Wang, Jia, Chaojiang Zhang, Joshua H. Marks, and Ralf I. Kaiser. "Formation of All Three C2H4O Isomers—Ethylene Oxide (c-C2H4O), Acetaldehyde (CH3CHO), and Vinyl Alcohol (CH2CHOH)—in Ethanol-containing Interstellar Analog Ices." Astrophysical Journal 984, no. 2 (2025): 138. https://doi.org/10.3847/1538-4357/adc308.

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Abstract Oxygen-containing complex organic molecules are key precursors to biorelevant compounds fundamental for the origins of life. However, the untangling of their interstellar formation mechanisms has just scratched the surface, especially for oxygen-containing cyclic molecules. Here, we present the first laboratory simulation experiments featuring the formation of all three C2H4O isomers—ethylene oxide (c–C2H4O), acetaldehyde (CH3CHO), and vinyl alcohol (CH2CHOH)—in low-temperature model interstellar ices composed of carbon monoxide (CO) and ethanol (C2H5OH). Ice mixtures were exposed to
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Abplanalp, Matthew J., and Ralf I. Kaiser. "On the formation of complex organic molecules in the interstellar medium: untangling the chemical complexity of carbon monoxide–hydrocarbon containing ice analogues exposed to ionizing radiation via a combined infrared and reflectron time-of-flight analysis." Physical Chemistry Chemical Physics 21, no. 31 (2019): 16949–80. http://dx.doi.org/10.1039/c9cp01793c.

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Schmidt, Fabian, Petra Swiderek, Tarek Scheele, and Jan H. Bredehöft. "Mechanisms of methyl formate production during electron-induced processing of methanol–carbon monoxide ices." Physical Chemistry Chemical Physics 23, no. 20 (2021): 11649–62. http://dx.doi.org/10.1039/d1cp01255j.

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A novel mechanism is proposed for the electron-induced production of methyl formate from CO and CH<sub>3</sub>OH which is relevant for interstellar ice chemistry. A key-step in this reaction is the formation of an intermediate CH<sub>3</sub>OCO radical.
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Kuznetsov, O. V., M. M. Evseev, E. A. Batrakova, and I. O. Antonov. "Ionization Energy of Reaction Products in an Ethanol–Carbon Monoxide System in Interstellar Ices." Bulletin of the Lebedev Physics Institute 51, no. 3 (2024): 77–82. http://dx.doi.org/10.3103/s1068335623601826.

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Pilling, Sergio, Eduardo Seperuelo Duarte, Enio F. da Silveira, et al. "Radiolysis of ammonia-containing ices by heavy cosmic rays inside dense molecular clouds." Proceedings of the International Astronomical Union 5, S265 (2009): 442–43. http://dx.doi.org/10.1017/s1743921310001237.

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AbstractWe present experimental studies on the interaction of heavy, highly charged and energetic ions (46 MeV 58Ni13+) with interstellar ammonia-containing (H2O:NH3:CO) ice analog in an attempt to simulate the physical chemistry induced by heavy ion cosmic rays inside dense astrophysical environments. The measurements were performed at the heavy ion accelerator GANIL in Caen, France. In-situ analysis have been performed by a Fourier transform infrared spectrometer. The averaged values for the dissociation cross section of water, ammonia and carbon monoxide are determined and the estimated hal
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Bennett, Chris J., Corey S. Jamieson, and Ralf I. Kaiser. "AN EXPERIMENTAL INVESTIGATION OF THE DECOMPOSITION OF CARBON MONOXIDE AND FORMATION ROUTES TO CARBON DIOXIDE IN INTERSTELLAR ICES." Astrophysical Journal Supplement Series 182, no. 1 (2009): 1–11. http://dx.doi.org/10.1088/0067-0049/182/1/1.

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Ioppolo, S., B. A. McGuire, M. A. Allodi, and G. A. Blake. "THz and mid-IR spectroscopy of interstellar ice analogs: methyl and carboxylic acid groups." Faraday Discuss. 168 (2014): 461–84. http://dx.doi.org/10.1039/c3fd00154g.

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A fundamental problem in astrochemistry concerns the synthesis and survival of complex organic molecules (COMs) throughout the process of star and planet formation. While it is generally accepted that most complex molecules and prebiotic species form in the solid phase on icy grain particles, a complete understanding of the formation pathways is still largely lacking. To take full advantage of the enormous number of available THz observations (e.g.,Herschel Space Observatory, SOFIA, and ALMA), laboratory analogs must be studied systematically. Here, we present the THz (0.3–7.5 THz; 10–250 cm<s
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Collings, M. P., J. W. Dever, M. R. S. McCoustra, and H. J. Fraser. "Implications of Ice Morphology for Comet Formation." Highlights of Astronomy 13 (2005): 491–94. http://dx.doi.org/10.1017/s1539299600016397.

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AbstractLaboratory surface science under ultra-high vacuum (UHV) conditions allows us to simulate the growth of ices in astrophysical environments. Using the techniques of temperature programmed desorption (TPD), reflection-absorption infrared spectroscopy (RAIRS) and micro-balance methods, we have studied binary ice systems consisting of water (H2O) and variety of other species including carbon monoxide (CO), at astrophysically relevant conditions of temperature and pressure. We present results that demonstrate that the morphology of water ice has an important influence on the behavior of suc
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Huang, C. H., A. Ciaravella, C. Cecchi-Pestellini, et al. "Effects of 150–1000 eV Electron Impacts on Pure Carbon Monoxide Ices Using the Interstellar Energetic-Process System (IEPS)." Astrophysical Journal 889, no. 1 (2020): 57. http://dx.doi.org/10.3847/1538-4357/ab5dbe.

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Tesis sobre el tema "Interstellar ices. carbon monoxide"

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Del, Fré Samuel. "Études théoriques de la photodésorption d'analogues de glaces moléculaires interstellaires : application au monoxyde de carbone." Electronic Thesis or Diss., Université de Lille (2022-....), 2024. http://www.theses.fr/2024ULILR039.

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Des quantités inhabituelles de molécules en phase gazeuse sont détectées dans les régions froides (environ 10 K) du milieu interstellaire (ISM), principalement attribuées à la désorption non thermique de molécules depuis les glaces déposées sur les grains de poussière. En particulier, la désorption induite par les rayons ultraviolets du vide (photodésorption VUV) est considérée comme étant une voie de désorption majoritaire dans les régions de l'ISM dominées par les photons. Les investigations expérimentales ont révélé que dans les glaces pures de monoxyde de carbone (CO), espèce omniprésente
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Letzelter, Corinne. "Spectroscopie et photodissociation de la molecule de co : applications astrophysiques." Paris 6, 1987. http://www.theses.fr/1987PA066182.

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Etude des spectres d'absorption et d'emission de la molecule de co et de ses isotopes dans le domaine 88. 5 nm-125 nm. Les sections efficaces d'absorption des bandes de co entre 88. 5 nm et 115 nm ont ete mesurees en utilisant le rayonnement synchrotron comme source lumineuse. La fluorescence a ete observee dans tout le domaine uv et visible et les rendements de flourescence ont ete determines. La section efficace de photodissociation corespondante est calculee en tenant compte d'un eventuel continuum de dissociation pour lequel une limite de la section efficace d'absorption a ete donnee. Pres
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3

Reynaud, Denis. "Dynamique du gaz interstellaire dans les galaxies spirales barrées : une étude en interférométrie millimétrique de NGC 1530." Université Joseph Fourier (Grenoble), 1998. http://www.theses.fr/1998GRE10044.

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Les barres jouent probablement un role important dans l'evolution des galaxies. Le potentiel gravitationnel de la barre est capable de concentrer de grandes quantites de gaz interstellaire dans le voisinage du noyau, fournissant ainsi du combustible aux activites nucleaires eventuelles (formation explosive d'etoiles ou disque d'accretion de trou noir). Le gaz tombe vers le centre de la galaxie le long de deux chocs presque paralleles a la barre. Ces chocs sont riches en poussieres et en gaz moleculaire. L'interferometre millimetrique et le telescope de 30m de l'iram ont permis une etude precis
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4

Jacq, Thierry. "Le survey radiomillimetrique de l'observatoire de bordeaux : le gaz moleculaire interstellaire dans le plan galactique entre l=38 et l=67.5, structure spirale, nuages moleculaires, comparaison entre hi et **(13)co. ch dans le nuage sombre lynds 134." Paris 6, 1987. http://www.theses.fr/1987PA066440.

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L'observation radiomillimetrique a 110. 2 ghz du plan galactique a permis d'identifier 181 nuages interstellaires dont certains parametres sont listes. Deux bras spiraux sont mis en evidence: celui de persee d'inclinaison 12**(o) et un bras mineur lie au gaz local et incline de 22**(o). Les donnees moleculaires sont correlees aux donnees hi obtenues a arecibo et les resultats de cette comparaison sont presentes. D'autre part le nuage sombre l 134 est observe a 9 cm en ch et l'abondance relative de ce radical en fonction de la position est determinee
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5

Pon, Andrew Richard. "Shocks, Superbubbles, and Filaments: Investigations into Large Scale Gas Motions in Giant Molecular Clouds." Thesis, 2013. http://hdl.handle.net/1828/4553.

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Giant molecular clouds (GMCs), out of which stars form, are complex, dynamic systems, which both influence and are shaped by the process of star formation. In this dissertation, I examine three different facets of the dynamical motions within GMCs. Collapse modes in different dimensional objects. Molecular clouds contain lower dimensional substructures, such as filaments and sheets. The collapse properties of finite filaments and sheets differ from those of spherical objects as well as infinite sheets and filaments. I examine the importance of local collapse modes of small central perturb
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Libros sobre el tema "Interstellar ices. carbon monoxide"

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Symposium, International Astronomical Union. CO: Twenty-five years of millimeter-wave spectroscopy : proceedings of the 170th Symposium of the International Astronomical Union, held in Tucson, Arizona, May 29-June 5, 1995. Kluwer Academic Publishers, 1997.

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2

United States. National Aeronautics and Space Administration. Scientific and Technical Information Branch., ed. Molecular clouds in Orion and Monoceros. National Aeronautics and Space Administration, Scientific and Technical Information Branch, 1986.

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Symposium, International Astronomical Union. CO, twenty-five years of millimeter-wave spectroscopy: Poster presentations, IAU Symposium 170, 29 May-2 June 1995, Tucson, Arizona. National Radio Astronomy Observatory, 1997.

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Symposium, International Astronomical Union. CO, twenty-five years of millimeter-wave spectroscopy: Proceedings of the 170th Symposium of the International Astronomical Union, held in Tucson, Arizona, May 29-June 5, 1995. Kluwer Academic Publishers, 1996.

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Molecular clouds in the Carmina arm. 1986.

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Molecular clouds in Orion and Monoceros. 1986.

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CO: Twenty-Five Years of Millimeter-Wave Spectroscopy (International Astronomical Union Symposia). Springer, 1996.

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Capítulos de libros sobre el tema "Interstellar ices. carbon monoxide"

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Kakkar, Harjasnoor, Berta Martínez-Bachs, and Albert Rimola. "An Ab Initio Computational Study of Binding Energies of Interstellar Complex Organic Molecules on Crystalline Water Ice Surface Models." In Computational Science and Its Applications – ICCSA 2022 Workshops. Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-031-10562-3_21.

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AbstractThe interstellar medium is extremely heterogeneous in terms of physical environments and chemical composition. Spectroscopic observations in the recent decades have revealed the presence of gaseous material and dust grains covered in ices predominantly of water in interstellar clouds, the interplay of which may elucidate the existence of more than 250 molecular species. Of these species of varied complexity, several terrestrial carbon-containing compounds have been discovered, known as interstellar complex organic molecules (iCOMs) in the astrochemical argot. In order to investigate th
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2

"Chemistry in the Freezer: Making Complex Molecules From Simple Interstellar Ices." In Dust in Galaxies. The Royal Society of Chemistry, 2019. http://dx.doi.org/10.1039/9781788015059-00132.

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In darker regions of interstellar clouds, dust grains accumulate layers of simple ices on their surfaces. These ices are composed mainly of water, but also contain carbon monoxide and dioxide, simple hydrides such as methane and ammonia, and a few other species. Many of these icy species are also formed in simple chemical reactions on the surfaces of dust grains and are retained there until the ices are removed. These ice layers are chemically simple, but are the raw material for forming relatively complex molecular species, especially in star-forming regions. The formation of complex species
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"Interstellar Carbon Monoxide." In The ALMA Telescope. Cambridge University Press, 2023. http://dx.doi.org/10.1017/9781009279727.003.

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Actas de conferencias sobre el tema "Interstellar ices. carbon monoxide"

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Karteyeva, V., R. Nakibov, M. Ozhiganov, M. Medvedev, and A. Vasyunin. "Laboratory study of the IR spectra of methane ices in the polar environment." In Modern astronomy: from the Early Universe to exoplanets and black holes. Special Astrophysical Observatory of the Russian Academy of Sciences, 2024. https://doi.org/10.26119/vak2024.062.

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We grew the pure methane ice and mixed binary ices of methane with polar molecules: water, carbon dioxide, methanol and ammonia under ultrahigh vacuum cryogenic conditions similar to those in cold prestellar clouds. The composition of ices was chosen to reflect current astrochemical notions. The following interstellar ice analogues were obtained: H$_2$O : CH$_4$ = 10 : 1, CO$_2$ : CH$_4$ = 5 : 1, CH$_3$OH : CH$_4$ = 2 : 1, NH$_3$ : CH$_4$ = 1 : 1, that are new to the literature and infrared spectra ice analogues databases. We report the significance of deposition temperature for the internal s
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2

Waller, Michael G., Mark R. Walluk, and Thomas A. Trabold. "Towards the Development of a Fuel Cell System for Residential Applications: Propane Reforming via Catalytic Partial Oxidation." In ASME 2014 12th International Conference on Fuel Cell Science, Engineering and Technology collocated with the ASME 2014 8th International Conference on Energy Sustainability. American Society of Mechanical Engineers, 2014. http://dx.doi.org/10.1115/fuelcell2014-6431.

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The Environmental Protection Agency (EPA) has estimated that 5% of air pollutants originate from small internal combustion engines (ICE) used in non-automotive applications. While there have been significant advances towards developing more sustainable systems to replace large ICEs, few designs have been implemented with the capability to replace small ICEs such as those used in the residential sector for lawn and garden equipment. Replacing these small residential internal combustion engines presents a unique opportunity for early market penetration of fuel cell technologies. This paper descr
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Baines, Kevin H., and W. Hayden Smith. "Adaptive spectropolarimetric imaging from the Cassini orbiter." In OSA Annual Meeting. Optica Publishing Group, 1989. http://dx.doi.org/10.1364/oam.1989.thn1.

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Ambitious objectives for the NASA/ESA Cassini orbiter/Titan probe mission to the saturnian system include the determination of composition and distribution of material within rings, on satellite surfaces, and within the atmospheres of Saturn and Titan. Dynamic processes which lead to spatial and temporal variations are also to be investigated. Known materials include hydrogen, methane, ammonia, phosphine, germane, and carbon monoxide for Saturn; nitrogen, methane, and higher hydrocarbons for Titan; and water and possibly ammonia ice for the other satellites and rings. Within atmospheres, ammon
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