Relevant bibliographies by topics / Interstellar Atmosphere Chemistry

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers

Academic literature on the topic 'Interstellar Atmosphere Chemistry'

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Published: 7 September 2023

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Journal articles on the topic "Interstellar Atmosphere Chemistry"

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Phillips, T. G., Ewine F. Van Dishoeck, and Jocelyn B. Keene. "Interstellar H3O+." Symposium - International Astronomical Union 150 (1992): 191–92. http://dx.doi.org/10.1017/s0074180900089993.

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The H3O+ ion is a key species in the oxygen chemistry leading to H2O, OH and O2. Chemical models predict O2 and H2O to be the dominant oxygen-bearing molecules in interstellar clouds. However, neither of them can easily be observed in the bulk of the interstellar medium because of blockage from the Earth's atmosphere. Determination of the abundance and distribution of the precursor H3O+ ion might thus provide an important indirect measure of their abundances.
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Peacock, Sarah, Travis S. Barman, Adam C. Schneider, Michaela Leung, Edward W. Schwieterman, Evgenya L. Shkolnik, and R. O. Parke Loyd. "Accurate Modeling of Lyα Profiles and Their Impact on Photolysis of Terrestrial Planet Atmospheres." Astrophysical Journal 933, no. 2 (July 1, 2022): 235. http://dx.doi.org/10.3847/1538-4357/ac77f2.

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Abstract Accurately measuring and modeling the Lyα (Lyα; λ1215.67 Å) emission line from low-mass stars is vital for our ability to build predictive high energy stellar spectra, yet interstellar medium (ISM) absorption of this line typically prevents model-measurement comparisons. Lyα also controls the photodissociation of important molecules, like water and methane, in exoplanet atmospheres such that any photochemical models assessing potential biosignatures or atmospheric abundances require accurate Lyα host star flux estimates. Recent observations of three early M and K stars (K3, M0, M1) with exceptionally high radial velocities (>100 km s−1) reveal the intrinsic profiles of these types of stars as most of their Lyα flux is shifted away from the geocoronal line core and contamination from the ISM. These observations indicate that previous stellar spectra computed with the PHOENIX atmosphere code have underpredicted the core of Lyα in these types of stars. With these observations, we have been able to better understand the microphysics in the upper atmosphere and improve the predictive capabilities of the PHOENIX atmosphere code. Since these wavelengths drive the photolysis of key molecular species, we also present results analyzing the impact of the resulting changes to the synthetic stellar spectra on observable chemistry in terrestrial planet atmospheres.
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Barnett, NeilW. "Spectroscopy of the Earth's Atmosphere and Interstellar Medium." Analytica Chimica Acta 284, no. 1 (December 1993): 241. http://dx.doi.org/10.1016/0003-2670(93)80030-o.

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Willacy, Karen, SiHe Chen, Danica J. Adams, and Yuk L. Yung. "Vertical Distribution of Cyclopropenylidene and Propadiene in the Atmosphere of Titan." Astrophysical Journal 933, no. 2 (July 1, 2022): 230. http://dx.doi.org/10.3847/1538-4357/ac6b9d.

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Abstract Titan’s atmosphere is a natural laboratory for exploring the photochemical synthesis of organic molecules. Significant recent advances in the study of the atmosphere of Titan include: (a) detection of C3 molecules: C3H6, CH2CCH2, c-C3H2, and (b) retrieval of C6H6, which is formed primarily via C3 chemistry, from Cassini Ultraviolet Imaging Spectrograph data. The detection of c-C3H2 is of particular significance as ring molecules are of great astrobiological importance. Using the Caltech/JPL KINETICS code, along with the best available photochemical rate coefficients and parameterized vertical transport, we are able to account for the recent observations. It is significant that ion chemistry, reminiscent of that in the interstellar medium, plays a major role in the production of c-C3H2 above 1000 km.
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Smith, David, and Patrik Spanel. "Ions in the terrestrial atmosphere and in interstellar clouds." Mass Spectrometry Reviews 14, no. 4-5 (July 1995): 255–78. http://dx.doi.org/10.1002/mas.1280140403.

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Rimmer, Paul B., Catherine Walsh, and Christiane Helling. "Cosmic Rays, UV Photons, and Haze Formation in the Upper Atmospheres of Hot Jupiters." Proceedings of the International Astronomical Union 8, S299 (June 2013): 303–4. http://dx.doi.org/10.1017/s1743921313008703.

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AbstractCosmic ray ionization has been found to be a dominant mechanism for the formation of ions in dense interstellar environments. Cosmic rays are further known to initiate the highly efficient ion-neutral chemistry within star forming regions. In this talk we explore the effect of both cosmic rays and UV photons on a model hot Jupiter atmosphere using a non-equlibrium chemical network that combines reactions from the UMIST Database for Astrochemistry, the KIDA database for interstellar and protoplanetary environments and three-body and combustion reactions from the NIST database and from various irradiated gas planet networks. The physical parameters for our model atmosphere are based on HD 189733 b (Effective Temperature of 1000 K, log g = 3.3, solar metallicity, at a distance 0.03 AU from a K dwarf). The active UV photochemistry high in our model hot Jupiter atmosphere tends to destroy these hydrocarbons, but on a time-scale sufficiently slow that PAH formation could already have taken place. In most cases, carbon-bearing species formed by cosmic rays are destroyed by UV photons (e.g. C2H2, C2H4, HC3N). Conversely, carbon-bearing species enhanced by an active photochemistry are depleted when cosmic ray ionization is significant (e.g. CN, HCN and CH4). Ammonia is an interesting exception to this trend, enhanced both by an active photochemistry and a high cosmic ray ionization rate.
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Malmqvist, Per-Åke. "The RASSCF, RASSI, and CASPT2 Methods Used on Small Molecules of Astrophysical Interest." International Astronomical Union Colloquium 146 (1994): 338–52. http://dx.doi.org/10.1017/s0252921100021448.

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To a quantum chemist with no particular background in astrophysics or astronomy, a brief glance at journals and textbooks in these fields shows at least three areas where computational quantum chemistry has had a valuable impact: Interstellar cloud chemistry; stellar atmosphere modelling; and chemistry in extreme conditions, such as at the surface of a neutron star. The first two uses are particularly suitable, since standard methods are directly applicable.For such problems, good calculations of potential energy as well as expectation values and matrix elements of dipole and other operators appears to be in demand. Many electronic states may be involved, at least a broad range of problems involve fairly small molecules, often radicals, and conformation regions far from equilibrium. Such problems are addressed by three methods originated in our laboratory, and known by the acronyms RASSCF (Restricted Active Space Self-Consistent Field, Malmqvist et al. 1990), RASSI (RAS State Interaction) and CASPT2 (Complete Active Space Perturbation Theory to Second Order-Complete Active Space Perturbation Theory to Second Order, Andersson et al. 1990; Andersson et al. 1992).
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Notsu, Shota, Christian Eistrup, Catherine Walsh, and Hideko Nomura. "The composition of hot Jupiter atmospheres assembled within chemically evolved protoplanetary discs." Monthly Notices of the Royal Astronomical Society 499, no. 2 (September 25, 2020): 2229–44. http://dx.doi.org/10.1093/mnras/staa2944.

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ABSTRACT The radial-dependent positions of snowlines of abundant oxygen- and carbon-bearing molecules in protoplanetary discs will result in systematic radial variations in the carbon-to-oxygen (C/O) ratios in the gas and ice. This variation is proposed as a tracer of the formation location of gas-giant planets. However, disc chemistry can affect the C/O ratios in the gas and ice, thus potentially erasing the chemical fingerprint of snowlines in gas-giant atmospheres. We calculate the molecular composition of hot Jupiter atmospheres using elemental abundances extracted from a chemical kinetics model of a disc mid-plane, where we have varied the initial abundances and ionization rates. The models predict a wider diversity of possible atmospheres than those predicted using elemental ratios from snowlines only. As found in previous work, as the C/O ratio exceeds the solar value, the mixing ratio of CH4 increases in the lower atmosphere, and those of C2H2 and HCN increase mainly in the upper atmosphere. The mixing ratio of H2O correspondingly decreases. We find that hot Jupiters with C/O > 1 can only form between the CO2 and CH4 snowlines. Moreover, they can only form in a disc which has fully inherited interstellar abundances, and where negligible chemistry has occurred. Hence, carbon-rich planets are likely rare, unless efficient transport of hydrocarbon-rich ices via pebble drift to within the CH4 snowline is a common phenomenon. We predict combinations of C/O ratios and elemental abundances that can constrain gas-giant planet formation locations relative to snowline positions, and that can provide insight into the disc chemical history.
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Bergin, Edwin A., Geoffrey A. Blake, Fred Ciesla, Marc M. Hirschmann, and Jie Li. "Tracing the ingredients for a habitable earth from interstellar space through planet formation." Proceedings of the National Academy of Sciences 112, no. 29 (July 6, 2015): 8965–70. http://dx.doi.org/10.1073/pnas.1500954112.

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We use the C/N ratio as a monitor of the delivery of key ingredients of life to nascent terrestrial worlds. Total elemental C and N contents, and their ratio, are examined for the interstellar medium, comets, chondritic meteorites, and terrestrial planets; we include an updated estimate for the bulk silicate Earth (C/N = 49.0 ± 9.3). Using a kinetic model of disk chemistry, and the sublimation/condensation temperatures of primitive molecules, we suggest that organic ices and macromolecular (refractory or carbonaceous dust) organic material are the likely initial C and N carriers. Chemical reactions in the disk can produce nebular C/N ratios of ∼1–12, comparable to those of comets and the low end estimated for planetesimals. An increase of the C/N ratio is traced between volatile-rich pristine bodies and larger volatile-depleted objects subjected to thermal/accretional metamorphism. The C/N ratios of the dominant materials accreted to terrestrial planets should therefore be higher than those seen in carbonaceous chondrites or comets. During planetary formation, we explore scenarios leading to further volatile loss and associated C/N variations owing to core formation and atmospheric escape. Key processes include relative enrichment of nitrogen in the atmosphere and preferential sequestration of carbon by the core. The high C/N bulk silicate Earth ratio therefore is best satisfied by accretion of thermally processed objects followed by large-scale atmospheric loss. These two effects must be more profound if volatile sequestration in the core is effective. The stochastic nature of these processes hints that the surface/atmospheric abundances of biosphere-essential materials will likely be variable.
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Wang, Zhe-Chen, Callie A. Cole, Nicholas J. Demarais, Theodore P. Snow, and Veronica M. Bierbaum. "Reactions of Azine Anions with Nitrogen and Oxygen Atoms: Implications for Titan’s Upper Atmosphere and Interstellar Chemistry." Journal of the American Chemical Society 137, no. 33 (August 17, 2015): 10700–10709. http://dx.doi.org/10.1021/jacs.5b06089.

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Dissertations / Theses on the topic "Interstellar Atmosphere Chemistry"

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Jamal, Eddine Nour. "Reactivity of molecular anions at low temperature : implications for the chemistry of the interstellar medium ant Titan's atmosphere." Thesis, Rennes 1, 2017. http://www.theses.fr/2017REN1S132/document.

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Depuis leur découverte dans divers environnements astrophysiques, les anions polyyne CxH¯ (x = 2, 4, 6) et les anions cyanopolyyne CxN¯ (x = 1, 3, 5) ont reçu une attention considérable. Ces anions semblent jouer des rôles importants dans leur environnement. Cependant, les données à basse température sur les voies chimiques menant à leur formation et à leur destruction sont encore rares, en particulier ce qui concerne l'identité du produit et les ratios de ramification. Pour résoudre ce problème, nous nous sommes engagés dans la recherche de la réactivité de ces anions moléculaires en utilisant des instruments dédiés couplant des jets subsonique et supersonique avec des méthodes de spectrométrie de masse. De cette façon, nous avons étudié la réactivité des anions C3N avec le cyanoacétylène (HC3N) ainsi que la réactivité de CN¯, C3N¯, et C5N¯ avec l'acide formique (HCOOH) de 298 K à des températures aussi basses que 36 K. Nous rapportons dans ce travail le taux de vitesse, les produits, et les ratios de ramification de ces réactions. Ce travail aborde également la source prototype d'ions sélectionnée, qui a récemment été mis en place dans notre laboratoire afin d'étendre notre recherche à d'autres anions d'intérêt astrophysique (e.g. les anions CxH¯ et Cx¯). Une description de cet instrument ainsi que des résultats préliminaires sont présentés dans ce travail. Cette thèse, «Reactivity of Molecular Anions at Low Temperature: Implications for the Chemistry of the Interstellar medium and Titan’s atmosphere», a été réalisée au sein de l'Institut de physique de Rennes et de l'Ecole Nationale Supérieure de Chimie de Rennes. Mots-clés: astrochimie, atmosphère de Titan, anions moléculaires, cinétique en phase gazeuse, jet supersonique, spectrométrie de masse, source d’ions sélectionnée
Ever since their discovery in various astrophysical environments, polyyne anions CxH¯ (x = 2, 4, 6) and cyanopolyyne anions CxN¯ (x = 1, 3, 5) have received a considerable attention. These anions appear to be playing important roles in their environments. However, low temperature data on the chemical pathways leading to their formation and destruction is still scarce, especially regarding product identity and branching ratios. To address this issue, we have engaged in the investigation of the reactivity of these molecular anions by employing dedicated instruments coupling subsonic and supersonic flows with mass spectrometry methods. In this fashion, we have investigated the reactivity of C3N¯ anions with cyanoacetylene (HC3N) as well as the reactivity of CN¯, C3N¯, and C5N¯ with formic acid (HCOOH) from 298 K down to temperatures as low as 36 K. We report in this work the rate coefficient, the nature of the products, and the branching ratios of these reactions.This work also addresses the prototype selected ion source in our laboratory, which was recently implemented in order to extend our investigation to other anions of astrophysical interest (e.g. CxH¯ and Cx¯ anions). A description of this instrument as well as some preliminary results are presented in this work. This thesis, «Reactivity of Molecular Anions at Low Temperature: Implications for the Chemistry of the Interstellar medium and Titan’s atmosphere», was carried out at the Institut de Physique de Rennes and the Ecole Nationale Supérieure de Chimie de Rennes.Keywords: astrochemistry, Titan’s atmosphere, molecular anions, gas phase kinetics, supersonic flow, mass spectrometry, selected ion source
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Landera, Alexander. "Formation of Polycyclic Aromatic Hydrocarbons and Nitrogen Containing Polcyclic Aromatic Compounds in Titan's Atmosphere, the Interstellar Medium and Combustion." FIU Digital Commons, 2013. http://digitalcommons.fiu.edu/etd/991.

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Several different mechanisms leading to the formation of (substituted) naphthalene and azanaphthalenes were examined using theoretical quantum chemical calculations. As a result, a series of novel synthetic routes to Polycyclic Aromatic Hydrocarbons (PAHs) and Nitrogen Containing Polycyclic Aromatic Compounds (N-PACs) have been proposed. On Earth, these aromatic compounds originate from incomplete combustion and are released into our environment, where they are known to be major pollutants, often with carcinogenic properties. In the atmosphere of a Saturn’s moon Titan, these PAH and N-PACs are believed to play a critical role in organic haze formation, as well as acting as chemical precursors to biologically relevant molecules. The theoretical calculations were performed by employing the ab initio G3(MP2,CC)/B3LYP/6-311G** method to effectively probe the Potential Energy Surfaces (PES) relevant to the PAH and N-PAC formation. Following the construction of the PES, Rice-Ramsperger-Kassel-Markus (RRKM) theory was used to evaluate all unimolecular rate constants as a function of collision energy under single-collision conditions. Branching ratios were then evaluated by solving phenomenological rate expressions for the various product concentrations. The most viable pathways to PAH and N-PAC formation were found to be those where the initial attack by the ethynyl (C2H) or cyano (CN) radical toward a unsaturated hydrocarbon molecule led to the formation of an intermediate which could not effectively lose a hydrogen atom. It is not until ring cyclization has occurred, that hydrogen elimination leads to a closed shell product. By quenching the possibility of the initial hydrogen atom elimination, one of the most competitive processes preventing the PAH or N-PAC formation was avoided, and the PAH or N-PAC formation was allowed to proceed. It is concluded that these considerations should be taken into account when attempting to explore any other potential routes towards aromatic compounds in cold environments, such as on Titan or in the interstellar medium.
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Blanksby, Stephen J. ""Gas phase synthesis of interstellar cumulenes : mass spectrometric and theoretical studies" /." Title page, contents and summary only, 1999. http://web4.library.adelaide.edu.au/theses/09PH/09phb6423.pdf.

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Thesis (Ph.D.)-- University of Adelaide, Dept. of Chemistry, 1999.
Copies of author's previously published articles inserted. Supplement entitled: Addressing referee concerns, stapled to back end paper (5 leaves). Bibliography: leaves 199-212.
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Vásquez, Mencos Abraham Alejandro. "The Nitrogen Chemistry in Solid Phase at Cryogenic Temperatures : Molecular Evolutions in Interstellar Clouds and Planetary Atmospheres." Thesis, Sorbonne université, 2018. http://www.theses.fr/2018SORUS256.

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L'azote est le cinquième élément le plus abondant de l'Univers, et les réservoirs les plus importants de cet élément sont les nuages moléculaires et les disques proto-planétaires. En raison des conditions du milieu interstellaire, la majeure partie de l'azote existe sous forme atomique. Bien que les espèces azotées soient très abondantes dans le milieu interstellaire et dans certaines atmosphères planétaires et cométaires, peu d’études de laboratoire ont été réalisées visant à comprendre le rôle d'azote atomique dans la chimie de ces régions de l'Univers. Dans cette thèse, nous avons exploré la réactivité, en phase solide et aux températures cryogéniques, de l'azote atomique à l’état fondamental N(4S) avec des composés organiques simple comme CH4 et CH3CN. Les réactifs, produits et intermédiaires de réaction sont sondés in situ par spectroscopie infrarouge à transformée de Fourier (IRTF). Nous avons montré, dans une première étape, que le chauffage progressif de nos échantillons solides entre 3 et 10 K, stimule la recombinaison atomique N(4S) - N(4S) et la formation de formes excités de l'azote atomique et moléculaire, N2(A) et N(2D). Ces espèces sont très réactives et jouent un rôle essentiel dans la dissociation de composés organiques. Dans une seconde étape, le chauffage continu de 10 à 40 K induit principalement des recombinaisons des radicaux formés dans la première étape conduisant à la formation de molécules organiques complexes comme NH3, C2H6, HCN et HNC. Ces travaux de recherche décrivent le rôle de l'azote atomique en phase solide des nuages moléculaires comme étant très semblable à celui des rayonnements UV dans les nuages diffus
Nitrogen is the fifth most abundant element in the Universe, and the most significant reservoirs of this element are molecular clouds, dark clouds, and proto-planetary discs. Due to the conditions of the interstellar medium, most of the nitrogen exists in atomic form. Even the enormous abundance of this element there are not many studies aimed at understanding the role that nitrogen plays in the chemistry of dark molecular clouds and other cold regions of the Universe where the UV light and other energetic particles are not able to penetrate. In the present Ph-D thesis, we have explored the reactivity of atomic nitrogen in ground state N(4S) thermally induced with small organic compounds in the solid phase at cryogenic temperatures from 3 to 40K using Fourier Transform Infrared Spectroscopy (FTIR) analysis. We have shown that gradual heating in a first step, between 3 and 10K, stimulates N(4S) - N(4S) recombination and the consequent formation of the excited forms of nitrogen N2(A) and N(2D). These species play an essential role in the dissociation of H-C bearing species to form radicals. Then, in a second step, the continuous heating from 10 to 40K, induces the recombination of the radicals formed in the first step to produce more stable and complex compounds. During this process, there are observed reactions of addition, H-elimination, C-N, C-C formation, molecular fragmentation and isomerization. From these experiments, we have demonstrated that role of atomic nitrogen in dark molecular clouds is equivalent to that of UV light in diffuse clouds
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Blanksby, Stephen J. (Stephen James). ""Gas phase synthesis of interstellar cumulenes : mass spectrometric and theoretical studies" / by Stephen J. Blanksby." 1999. http://hdl.handle.net/2440/19402.

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Copies of author's previously published articles inserted.
Supplement entitled: Addressing referee concerns, stapled to back end paper (5 leaves).
Bibliography: leaves 199-212.
xii, 212 leaaves : ill. ; 30 cm.
Title page, contents and abstract only. The complete thesis in print form is available from the University Library.
Presents methodologies for the synthesis of charged analogues of a number of molecular species residing in the large gas clouds which are present in regions of interstellar and circumstellar space. Quantum chemical calculations have been used to provide further insight into the structure and energetics of these molecules.
Thesis (Ph.D.)--University of Adelaide, Dept. of Chemistry, 1999
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Blanksby, Stephen J. (Stephen James). ""Gas phase synthesis of interstellar cumulenes : mass spectrometric and theoretical studies" / by Stephen J. Blanksby." Thesis, 1999. http://hdl.handle.net/2440/19402.

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Abstract:
Copies of author's previously published articles inserted.
Supplement entitled: Addressing referee concerns, stapled to back end paper (5 leaves).
Bibliography: leaves 199-212.
xii, 212 leaaves : ill. ; 30 cm.
Presents methodologies for the synthesis of charged analogues of a number of molecular species residing in the large gas clouds which are present in regions of interstellar and circumstellar space. Quantum chemical calculations have been used to provide further insight into the structure and energetics of these molecules.
Thesis (Ph.D.)--University of Adelaide, Dept. of Chemistry, 1999
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Books on the topic "Interstellar Atmosphere Chemistry"

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Krasnopolʹskiĭ, V. A. Photochemistry of Triton's atmosphere and ionosphere. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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Krasnopolʹskiĭ, V. A. Photochemistry of Triton's atmosphere and ionosphere. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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Symposium, COSPAR Scientific Commission F. F3 1. Life sciences: new insights into complex organics in space: Proceedings of the F3.1 Symposium of COSPAR Scientific Commission F which was held during the thirty-second COSPAR Scientific Assembly, Nagoya, Japan, 12-19 July, 1998. Oxford: Pergamon [for the] Committee on Space Research, 1999.

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Assembly, COSPAR Scientific. Life sciences: Complex organics in space : proceedings of the F3.2 symposium of COSPAR Scientific Commission F which was held during the thirty-first COSPAR scientific assembly, Birmingham, U.K., 14-21 July 1996. Kidlington, Oxford: Published for the Committee on Space Research [by] Pergamon, 1997.

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Assembly, COSPAR Scientific. Life sciences: Recent dosimetry results, chromosome damage and heritable effects : proceedings of the F2.6 and F2.9 symposia of COSPAR Scientific Commission F which was held during the thirty-first COSPAR Scientific Assembly, Birmingham, U.K., 14-21 July 1996. Kidlington, Oxford: Published for the Committee on Space Research [by] Pergamon, 1998.

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M, Wheeler R., and COSPAR Scientific Commission F, eds. Life sciences: Life support system studies-I : proceedings of the F4.6, F4.8, F4.2 and F4.9 symposia of COSPAR Scientific Commission F which was held during the thirty-first COSPAR Scientific Assembly, Birmingham, U.K., 14-21 July 1996. Oxford, [England]: Published for the Committee on Space Research [by] Pergamon, 1997.

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Assembly, COSPAR Scientific. Life sciences: Exobiology : proceedings of the F3.1, F3.3, F3.4 and F3.5 symposia of COSPAR Scientific Commission F which were held during the thirty-first COSPAR Scientific Assembly, Birmingham, U.K., 14-21 July 1996. Kidlington, Oxford: Published for the Committee on Space Research [by] Pergamon, 1998.

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Assembly, COSPAR Scientific. Life sciences: Exobiology : proceedings of the F3.3 and F3.5 symposia of COSPAR Scientific Commission F which was held during the thirty-second COSPAR Scientific Assembly, Nagoya, Japan, 12-19 July, 1998. Oxford: Published for the Committee on Space Research [by] Pergamon, 1999.

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Assembly, COSPAR Scientific. Life sciences: Space and Mars recent results : proceedings of the F3.1, F3.4, F2.4 and F3.8 Symposia of COSPAR Scientific Commission F, which were held during the Thirtieth COSPAR Scientific Assembly, Hamburg, Germany, 11-21 July, 1994. Oxford, UK: Published for the Committee on Space Research [by] Pergamon, 1996.

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Assembly, COSPAR Scientific. Life sciences: Space flight and the central nervous system : the potential independent and synergistic effects of microgravity and radiation : proceedings of the F2.4 Symposium of COSPAR Scientific Commission F which was held during the Thirty-first COSPAR Scientific Assembly, Birmingham, U.K., 14-21 July 1996. Oxford: Published for the Committee on Space Research [by] Pergamon, 1998.

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Book chapters on the topic "Interstellar Atmosphere Chemistry"

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Zalasiewicz, Jan. "100 Million Years AD." In The Earth After Us. Oxford University Press, 2008. http://dx.doi.org/10.1093/oso/9780199214976.003.0007.

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A storyteller arrives, one hundred million years from now, to tell the tale of the human species. It is an interval that will add a couple of per cent to the age of the Earth and a little under one per cent to the age of the Universe. Geologically, it is the near future. Cosmologically, we are almost there. There will be an Earth, that which we now call our own. On it there will be, very probably but not quite certainly, oceans of liquid water, an oxygen-rich atmosphere, and an abundance of complex, multicellular life. The Earth is abnormal, and that will draw any interstellar travellers in. The spaceship’s sensors—a simple spectroscope will suffice here—will immediately register the highly reactive surface chemistry that is out of any sort of normal equilibrium. An oxygen-rich atmosphere is not normal. Even from a distance of many millions of miles, this will be a planet that is obviously alive. Closer up, the living skin on the planet, regulator of that planetary surface chemistry, can begin to be glimpsed, as the green wavelengths that mingle with the blue of the oceans of liquid water and the brown of the rock surfaces. Our future visitors would not yet be aware of chlorophyll, but that unexpected signal shining through in the light spectrum would certainly arouse their curiosity. Rock, oceans . . . and green stuff. The geography of the Earth, to our own human and contemporary eyes, would look oddly familiar, but distorted: as though remodelled by Salvador Dali. Familiar landmasses will be displaced. But where to? Unfortunately, we cannot predict where the Earth’s continents will be in one hundred million years’ time. Will the Atlantic Ocean continue to widen, and the Pacific Ocean shrink? Will the East African Rift expand into an ocean? Will the continents aggregate into super-continents, as has happened in the past? Long-term tectonic forecasts, like long-range weather forecasts, are subject to such uncertainties that detailed prediction becomes useless; there are simply too many possible alternative futures. Our planet’s physiography will simply be different, one hundred million years from now, though with elements we would find partly familiar, rearranged as though by the hand of some gigantic and playful child.
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IRVINE, W. M., and R. F. KNACKE. "THE CHEMISTRY OF INTERSTELLAR GAS AND GRAINS." In Origin and Evolution of Planetary and Satellite Atmospheres, 3–34. University of Arizona Press, 1989. http://dx.doi.org/10.2307/j.ctv20dsb5m.5.

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Conference papers on the topic "Interstellar Atmosphere Chemistry"

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KLEMPERER, WILLIAM. "SOME THOUGHTS ON INTERSTELLAR CHEMISTRY." In Contributions to Atomic, Molecular, and Optical Physics, Astrophysics, and Atmospheric Physics. PUBLISHED BY IMPERIAL COLLEGE PRESS AND DISTRIBUTED BY WORLD SCIENTIFIC PUBLISHING CO., 2009. http://dx.doi.org/10.1142/9781848164703_0006.

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THADDEUS, PATRICK. "STILL MORE THOUGHTS ON INTERSTELLAR CHEMISTRY." In Contributions to Atomic, Molecular, and Optical Physics, Astrophysics, and Atmospheric Physics. PUBLISHED BY IMPERIAL COLLEGE PRESS AND DISTRIBUTED BY WORLD SCIENTIFIC PUBLISHING CO., 2009. http://dx.doi.org/10.1142/9781848164703_0011.

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HARTQUIST, T. W., S. VAN LOO, and S. A. E. G. FALLE. "HOW INTERSTELLAR CHEMISTRY (AND ASTROCHEMISTRY MORE GENERALLY) BECAME USEFUL." In Contributions to Atomic, Molecular, and Optical Physics, Astrophysics, and Atmospheric Physics. PUBLISHED BY IMPERIAL COLLEGE PRESS AND DISTRIBUTED BY WORLD SCIENTIFIC PUBLISHING CO., 2009. http://dx.doi.org/10.1142/9781848164703_0012.

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Morin, P. "Free Electron Laser Induced Dissociation of Molecules Probed with Synchrotron Radiation." In Free-Electron Laser Applications in the Ultraviolet. Washington, D.C.: Optica Publishing Group, 1988. http://dx.doi.org/10.1364/fel.1988.wc2.

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Abstract:
Photodissociation of isolated polyatomic molecules is of great interest not only for itself but also because it is closely related to various important areas such as photochemistry (1), combustion phenomena (2), atmospheric pollution (3), interstellar chemistry (4) and isotope separation (5). Considerable progresses was made in the 70's by the extensive use of lasers for a very selective excitation of the molecule. State to state correlations between the various steps of dissociation dynamics have been achieved by a combination of various techniques to probe the dissociation products., such as laser induced fluorescence (6), VUV ionization (4), resonant multiphoton ionization (7), coherent anti-stokes Raman spectroscopy (8), V_V transfert (9), IR or visible fluorescence (10) or mass spectrometry (11) associated with molecular beam technique. At this time, available lasers are not tunable over a wide range in the UV, thus limiting the species of molecules that can be studied.
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