Готові списки джерел за темами / Interstellar molecules

Добірка наукової літератури з теми "Interstellar molecules"

Автор: Grafiati
Опубліковано: 4 червня 2021
Оновлено: 6 вересня 2023

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Зміст

  1. Статті в журналах
  2. Дисертації
  3. Книги
  4. Частини книг
  5. Тези доповідей конференцій
  6. Звіти організацій

Статті в журналах з теми "Interstellar molecules":

1

Winnewisser, G., and E. Herbst. "Interstellar molecules." Reports on Progress in Physics 56, no. 10 (October 1, 1993): 1209–73. http://dx.doi.org/10.1088/0034-4885/56/10/001.

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2

Lequeux, J., and E. Roueff. "Interstellar molecules." Physics Reports 200, no. 5 (February 1991): 241–99. http://dx.doi.org/10.1016/0370-1573(91)90010-j.

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3

Kuan, Y. J., H. C. Huang, S. B. Charnley, W. L. Tseng, L. E. Snyder, P. Ehrenfreund, Z. Kisiel, S. Thorwirth, R. K. Bohn, and T. L. Wilson. "Prebiologically Important Interstellar Molecules." Symposium - International Astronomical Union 213 (2004): 185–88. http://dx.doi.org/10.1017/s0074180900193246.

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Understanding the organic chemistry of molecular clouds, particularly the formation of biologically important molecules, is fundamental to the study of the processes which lead to the origin, evolution and distribution of life in the Galaxy. Determining the level of molecular complexity attainable in the clouds, and the nature of the complex organic material available to protostellar disks and the planetary systems that form from them, requires an understanding of the possible chemical pathways and is therefore a central question in astrochemistry. We have thus searched for prebiologically important molecules in the hot molecular cloud cores: Sgr B2(N-LMH), W51 e1/e2 and Orion-KL. Among the molecules searched: Pyrimidine is the unsubstituted ring analogue for three of the DNA and RNA bases. 2H-Azirine and Aziridine are azaheterocyclic compounds. And Glycine is the simplest amino acid. Detections of these interstellar organic molecular species will thus have important implications for Astrobiology. Our preliminary results indicate a tentative detection of interstellar glycine. If confirmed, this will be the first detection of an amino acid in interstellar space and will greatly strengthen the thesis that interstellar organic molecules could have played a pivotal role in the prebiotic chemistry of the early Earth.
4

Kerridge, J. F. "Interstellar Molecules in Meteorites." Symposium - International Astronomical Union 135 (1989): 383–88. http://dx.doi.org/10.1017/s0074180900125392.

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Substantial enrichment of deuterium, D, in certain components of chondritic meteorites is interpreted as a record of isotopic fractionation during ion-molecule reactions at the very low temperatures characteristic of dense interstellar clouds. Whether those meteorites still contain the actual molecules that were synthesised in the presolar interstellar medium, or whether the interstellar material was recycled into a later generation of molecules within the early solar system is not known.
5

Menten, Karl M. "Interstellar methanol masers." Symposium - International Astronomical Union 206 (2002): 125–26. http://dx.doi.org/10.1017/s0074180900222213.

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The asymmetric rotor molecule methanol (CH3OH) has hundreds of transitions at centimeter-, millimeter-, and submillimeter wavelengths. Many of these are excited in the hot (T ≳ 150 K), dense (n ≳ 106 cm−3) molecular cloud cores surrounding newly formed massive stars or protostars. The high temperatures in these cores cause evaporation of icy grain mantles, releasing copious amounts of complex molecules, such as methanol, in the gas phase, which in hot cores has abundances (up to 10−6 relative to H2) that are two or more orders of magnitude higher than in cold dark clouds.
6

Kaźmierczak, Maja, Mirosław Schmidt, and Jacek Krełowski. "Dicarbon molecule in the interstellar clouds." Proceedings of the International Astronomical Union 4, S251 (February 2008): 45–46. http://dx.doi.org/10.1017/s1743921308021145.

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AbstractWe present high-resolution and high signal-to-noise spectroscopic observations of interstellar molecular lines of C2 towards early-type stars. C2 is particularly interesting because it is the simplest multicarbon molecule and its abundances give information on the chemistry of interstellar clouds, especially on the pathway of formation of (hydro)carbon chains and PAHs which may be considered as possible carriers of diffuse interstellar bands (DIBs). Homonuclear diatomic molecules have negligible dipol moments and hence radiative cooling of excited rotational levels may go only trough the slow quadrupole transitions (van Dishoeck & Black 1982). In C2, pumped by galactic average interstellar field rotational levels are excited effectively much above the gas kinetic temperature and a rotational ladder of electronic transitions is usually observed from high rotational levels. Relations between abundances of the dicarbon and other simple interstellar molecules are considered as well.
7

Ziurys, L. M., and B. E. Turner. "New Interstellar Molecular Detections: Implications for “Shock Chemistry”." Symposium - International Astronomical Union 120 (1987): 289–92. http://dx.doi.org/10.1017/s0074180900154166.

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Several new interstellar species have recently been detected in the molecular gas, including rotationally-excited CH, vibrationally-excited HCN, and a new molecular ion, HCNH+. These detections have raised some interesting questions concerning the relative importance of “shock” or “high temperature” chemistry vs. ion-molecule reactions in the synthesis of interstellar molecules in dense clouds.
8

Thaddeus, P. "The prebiotic molecules observed in the interstellar gas." Philosophical Transactions of the Royal Society B: Biological Sciences 361, no. 1474 (September 7, 2006): 1681–87. http://dx.doi.org/10.1098/rstb.2006.1897.

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Over 130 molecules have been identified in the interstellar gas and circumstellar shells, the largest among them is a carbon chain with 13 atoms and molecular weight of 147 (twice that of the simplest amino acid glycine). The high reliability of astronomical identifications, as well as the fairly accurate quantitative analysis which can often be achieved, is emphasized. Glycine itself has been claimed, but a recent analysis indicates that few, if any, of the astronomical radio lines attributed to glycine are actually from that molecule. Polycyclic aromatic hydrocarbons (PAHs) have long been proposed as the source of the unidentified infrared bands between 3 and 16 μm, but no single PAH has been identified in space, partly because PAHs generally have weak or non-existent radio spectra. A remarkable exception is the non-planar corannulene molecule (C 20 H 10 ) that has a strong radio spectrum; in the rich molecular cloud TMC-1, it is found that less than 10 −5 of the carbon is contained in this molecule, suggesting that PAHs are not the dominant large molecules in the interstellar gas, as has been claimed. Owing to inherent spectroscopic limitations, determining the structures of the large molecules in space may require capture of the dust grains, which are continually entering the outer Solar System.
9

Aiello, S., B. Barsella, C. Cecchi-Pestellini, F. Mencaraglia, and A. Rosolia. "Molecular Life-Time against Photodissociation in Dark Interstellar Clouds." Symposium - International Astronomical Union 120 (1987): 75–76. http://dx.doi.org/10.1017/s0074180900153811.

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Molecules in the interstellar space are exposed to interstellar radiation, so that they are destroyed by photodissociation processes, leading to the production of smaller molecules and ions, which in turn can react with other molecular species. Therefore, dissociation rates and dissociation products are important for the chemistry of interstellar molecules. This holds true also for relatively opaque and dense clouds (τ ≲ 10 in the visual), due to the multiple scattering of UV radiation by dust.
10

Min, Y. C. "ASTROCHEMISTRY AND INTERSTELLAR MOLECULES." Publications of The Korean Astronomical Society 25, no. 1 (March 31, 2010): 1–13. http://dx.doi.org/10.5303/pkas.2010.25.1.001.

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Статті в журналах Дисертації Книги

Дисертації з теми "Interstellar molecules":

1

Whelan, Mark Clifford. "Spectroscopic studies of interstellar molecules." Thesis, University of Sussex, 2017. http://sro.sussex.ac.uk/id/eprint/68548/.

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2

Couch, Philip Anthony. "Molecules in circumstellar and interstellar environments : TiO." Thesis, University of Nottingham, 2002. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.247564.

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3

Holland, Simon Michael. "Highly excited molecules and the interstellar maser." Thesis, University of Bristol, 1999. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.265469.

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4

Harada, Nanase. "Interstellar Molecules in Galactic and Extragalactic Sources." The Ohio State University, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=osu1312559226.

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5

Cernicharo, José. "Matiere diffuse et molecules interstellaires." Paris 7, 1988. http://www.theses.fr/1988PA077028.

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La structure des nuages sombres de la region taurus-auriga-perseus et les causes des differences chimiques observees sont etudiees a l'aide de donnees radio, ir et optique. Des observations millimetriques ont permis de realiser des cartes detaillees en co de ce complexe moleculaire interstellaire. De nouvelles molecules metalliques ont ete detectees (clna, clk, clal et fal) ainsi que des isotopes de sicc et hccch. Des travaux instrumentaux pour differents radiotelescopes sont aussi decrits
6

Quan, Donghui. "Chemical Modeling of Interstellar Molecules in Dense Cores." The Ohio State University, 2009. http://rave.ohiolink.edu/etdc/view?acc_num=osu1259614944.

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7

Vichetti, Rafael Mário [UNESP]. "Síntese dos isótopos do monóxido de carbono no meio interestelar." Universidade Estadual Paulista (UNESP), 2009. http://hdl.handle.net/11449/91889.

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Made available in DSpace on 2014-06-11T19:25:31Z (GMT). No. of bitstreams: 0 Previous issue date: 2009-12-21Bitstream added on 2014-06-13T19:53:20Z : No. of bitstreams: 1 vichietti_rm_me_rcla.pdf: 842604 bytes, checksum: 731ca276a75c1b92840e57bd7497b5e1 (MD5)
Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)
De acordo com os resultados observacionais de condensações de nuvens moleculares escuras, grandes variações na razão 13CO/C18O são observadas quando se comparam os resultados obtidos nas condensações situadas dentro da mesma nuvem, bem como de nuvem para nuvem. O valor médio dessa razão na condensação principal de Ophiuchus é inferior a 5. Por outro lado, o valor encontrado nas condensações que estão situadas ao norte de Oph é maior que 10. Grandes diferenças também são encontradas quando se comparam os resultados observacionais de diferentes nuvens escuras, tais como Ophiuchus e Taurus, onde são observados também um decréscimo da razão C18O/C17O com o aumento da densidade. Os processos químicos e físicos que governam essas variações ainda não estão claros. Nesse sentido, o objetivo da presente proposta é analisar a influência do colapso gravitacional de condensações de nuvens moleculares escuras na síntese das moléculas CO, C17O, C18O, 13CO, 13C17O e 13C18O. Tal análise é feita com base em comparações entre modelos que consideram diferentes condições entre si, tais como, tamanho da cadeia química, velocidade de colapso, densidade inicial e processos de congelamento de espécies químicas na superfície de grãos de poeira. Os resultados obtidos mostram que o tamanho da cadeia química tem influência nas razões 13CO/C18O e C18O/C17O, mas não tanto quanto a densidade inicial e a velocidade do colapso. Além disso, o congelamento das espécies químicas nos grãos é mais significativo nos estágios mais avançados da evolução da condensação. Os modelos de condensações escuras que sofrem colapso gravitacional lento e em queda livre reproduzem satisfatoriamente as razões 13CO/C18O e C18O/C17O observadas, o que permite concluir que o colapso gravitacional pode ter um importante efeito nas referidas razões.
According to the observational results of dark molecular clouds condensations, large variations in the ratio 13CO/C18O are observed when comparing the results obtained in the condensations located within the same cloud and cloud to cloud. The average value of this ratio in the main condensation of Ophiuchus is below 5. On the other hand, the value found in the condensations that are located north of Oph is larger than 10. Large differences are also found when comparing the observational results of different dark clouds such as Ophiuchus and Taurus, in which are also found a decrease of the C18O/C17O ratio with increasing density. The chemical and physical processes that govern these variations are still unclear. In this sense, the objective of this proposal is to analyze the influence of the gravitational collapse of centrally condensed clumps of dense molecular gas in the synthesis of the CO, C17O, C18O, 13CO, 13C17O and 13C18O molecules. This analysis is based on comparisons among models that consider different condition, such as, chemical chain, initial density, speed of collapse and freezing processes of the chemical species on the surface of dust grains. The results show that the size of the chemical chain has influence on the 13CO/C18O and C18O/C17O ratios, but they are not as important as the initial density and the speed of the collapse. Furthermore, the freezing of chemical species on the grains occurs at later times of the collapse. The models of a gravitational free-fall collapsing core and of slowly contracting core with higher initial density are consistent with observations. These results indicate that the gravitational collapse of molecular cores can have an important effect in the 13CO/C18O and C18O/C17O ratios.
8

Smith, Arfon. "Dust and molecules in interstellar, circumstellar and extragalactic environments." Thesis, University of Nottingham, 2006. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.438422.

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9

Doronin, Mikhail. "Adsorption on interstellar analog surfaces : from atoms to organic molecules." Thesis, Paris 6, 2015. http://www.theses.fr/2015PA066254/document.

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Les interactions gaz-grains jouent un rôle important dans la chimie des milieux interstellaires et protoplanétaires. Le paramètre-clé qui gouverne les échanges entre la surface des grains et la phase gazeuse est l’énergie d’adsorption Ea. Ce travail a pour but de développer une approche jointe expérimentale et théorique afin de déterminer les énergies d’adsorption pour des atomes et molécules d’intérêt astrophysique sur des substrats-modèles des surfaces des grains de poussière interstellaires. Expérimentalement, la méthode employée est la désorption programmée en température (TPD). Le travail a contribué en l’établissement d’une méthode de traitement des courbes de désorption, basée sur une distribution d’énergie d’adsorption et utilisant un set limité de données à plusieurs rampes de chauffage, pour déterminer le couple de paramètres de l’équation de Polanyi-Wigner que sont l’énergie d’adsorption et le préfacteur. D’un point de vue de la chimie théorique, les énergies d’adsorption sont déterminées en utilisant la théorie de la fonctionnelle de la densité (DFT) implémentée dans le module Vienna Ab initio Simulation Package (VASP). Cette méthode permet également d’accéder aux géométries d’adsorption, ainsi qu’aux différents sites sur la surface. La méthode expérimentale a été validée par une comparaison avec un système connu : l’adsorption du méthanol CH3OH sur le graphite. L’adsorption des gaz rares Ar/Kr/Xe sur les glaces d’eau a été étudiée comme un cas d’intérêt pour la planétologie. L’adsorption de l’acétonitrile (CH3CN) et de son isomère l’isoacétonitrile (CH3NC) sur les surfaces de graphite, de quartz et de glaces d’eau a également été étudiée, puisque ces deux molécules sont détectées dans le milieu interstellaire. Les énergies d'adsorption trouvées dans le cadre de ce travail seront intégrées dans la base des données KIDA
Gas-grain interaction plays an important role in the chemistry of the cold interstellar medium and protoplanetary disks. A key parameter for modeling the exchange between grain surfaces and gas phase is adsorption energy, Ea. This work aims to develop a reliable and systematic experimental/theoretical approach to determine the adsorption energies of relevant atoms and molecules on models of interstellar grain surfaces. Employed experimental technique is the Temperature Programmed Desorption. Developed experimental protocol and data treatment technique based on distribution of adsorption energies and use of a set of heating rates enable to determine the coupled parameters of Polanyi-Wigner equation: adsorption energy Ea and prefactor N. Computational chemistry approach, Density Functional Theory (DFT) as implemented in Vienna Ab initio Simulation Package (VASP) is used to get the insight on the behaviour of the surface-adsorbate systems at the atomic level. This approach allows as well to determine adsorption energies. A presence of multiple adsorption sites with different adsorption energies is predicted. Methanol CH3OH adsorption on graphite is used as a known example to validate the technique. Ar/Kr/Xe adsorption on water ice is studied as a case relevant for planetology. Acetonitrile (CH_3CN) and methyl isocyanide (CH_3NC) adsorption on water ice, quartz and graphite is investigated since those two molecules are both detected in the interstellar medium. Adsorption energies determined in this work will be included in KIDA database
10

Hunt, Maria, University of Western Sydney, of Science Technology and Environment College, and School of Engineering and Industrial Design. "Molecules in southern molecular clouds: a millimetre-wave study of dense cores." THESIS_CSTE_EID_Hunt_M.xml, 2001. http://handle.uws.edu.au:8081/1959.7/116.

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This thesis presents an observational study of molecular abundances in the dense cores of 27 prominent molecular clouds in the southern galactic plane.The molecular abundances and physical conditions in dense condensations have been derived from millimetre-wavelength observations of molecular rotational transitions.The study has produced a comprehensive data set of transition intensities and abundances for 10 different molecules in bright southern molecular clouds, and the general characteristics of emissions from these molecules such as optical depth, excitation and relative abundances are discussed. A comparison of different methods of calculating molecular hydrogen column density from observations of carbon monoxide emission is included.Both the analysis and the data collected provide an excellent starting point for further observational and theoretical studies of molecular clouds in the southern Milky Way utilising new instruments such as the millimeter-wave upgrade to the Australia Telescope Compact Array and the Attacama Large Millimetre Array (ALMA).
Doctor of Philosophy (PhD)
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Книги з теми "Interstellar molecules":

1

Yamada, Koichi M. T., and Gisbert Winnewisser, eds. Interstellar Molecules. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-16268-8.

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2

Yamada, Koichi M. T. Interstellar Molecules: Their Laboratory and Interstellar Habitat. Berlin, Heidelberg: Springer-Verlag Berlin Heidelberg, 2011.

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3

Suzuki, Hiroko. Toward interstellar chemistry: Works. Tokyo: National Astoronomy Observatory, 1989.

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4

K, Bohme Diethard, ed. Chemistry and spectroscopy of interstellar molecules. [Tokyo]: University of Tokyo Press, 1992.

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5

Flower, D. R. Molecular collisions in the interstellar medium. Cambridge [England]: Cambridge University Press, 1990.

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6

1974-, Haverkorn M., and Goss W. M, eds. SINS--small ionized and neutral structures in the diffuse interstellar medium: Proceedings of a workshop held at the National Radio Astronomy Observatory, Socorro, New Mexico, USA, 21-24 May 2006. San Francisco: Astronomical Society of the Pacific, 2007.

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7

Flynn, George. Theoretical molecular studies of astrophysical interest: 1 December 1974 - 30 September 1991 : final technical report. [Washington, DC: National Aeronautics and Space Administration, 1991.

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8

Symposium, International Astronomical Union. Triggered star formation in a turbulent interstellar medium: Proceedings of the 237th symposium of the International Astronomical Union held in Prague, Czech Republic August 14-18, 2006. Cambridge: Cambridge University Press, 2007.

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9

Masako, Suto, and United States. National Aeronautics and Space Administration., eds. Photoabsorption and photodissociation of molecules important in the interstellar medium. [Washington, DC: National Aeronautics and Space Administration, 1991.

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10

Masako, Suto, and United States. National Aeronautics and Space Administration., eds. Photoabsorption and photodissociation of molecules important in the interstellar medium: Annual report ... covering the period from 15 January 1988 to 14 January 1989. Washington, DC: NASA Headquarters, 1989.

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Частини книг з теми "Interstellar molecules":

1

Verschuur, Gerrit. "Interstellar Molecules." In Astronomers' Universe, 85–100. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-13422-2_7.

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2

Kaifu, Norio. "Interstellar Molecules." In Molecular Processes in Space, 205–31. Boston, MA: Springer US, 1990. http://dx.doi.org/10.1007/978-1-4613-0591-0_9.

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3

Maciel, Walter J. "Interstellar Molecules." In Astrophysics of the Interstellar Medium, 215–37. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-3767-3_10.

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4

Verschuur, Gerrit L. "Formation of Molecules." In Interstellar Matters, 248–57. New York, NY: Springer New York, 1989. http://dx.doi.org/10.1007/978-1-4612-4522-3_21.

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5

Wilson, Stephen. "Interstellar Molecules and Interstellar Chemistry." In Chemistry by Computer, 167–88. Boston, MA: Springer US, 1986. http://dx.doi.org/10.1007/978-1-4613-2137-8_8.

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6

Kerridge, J. F. "Interstellar Molecules in Meteorites." In Interstellar Dust, 383–88. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2462-8_34.

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7

Verschuur, Gerrit L. "Molecules and Interstellar Matter." In Interstellar Matters, 234–47. New York, NY: Springer New York, 1989. http://dx.doi.org/10.1007/978-1-4612-4522-3_20.

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8

Barker, John R., and Isabelle Cherchneff. "Grains, or Molecules? Thermal, or Non-Thermal?" In Interstellar Dust, 197–205. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2462-8_18.

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9

D’Hendecourt, L. B., A. Léger, P. Boissel, and F. X. Désert. "Infrared Emission Mechanism in Large Isolated Molecules." In Interstellar Dust, 207–19. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2462-8_19.

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10

Rohlfs, K., and T. L. Wilson. "Molecules in Interstellar Space." In Astronomy and Astrophysics Library, 360–427. Berlin, Heidelberg: Springer Berlin Heidelberg, 2004. http://dx.doi.org/10.1007/978-3-662-05394-2_14.

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Тези доповідей конференцій з теми "Interstellar molecules":

1

Thaddeus, Patrick. "Carbenes in the Interstellar Gas." In High Resolution Spectroscopy. Washington, D.C.: Optica Publishing Group, 1993. http://dx.doi.org/10.1364/hrs.1993.tha1.

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Carbenes are a significant trace constituent of the gas in the interstellar medium (and in the expanding shell around at least one star), representing about one-sixth of the molecular species that have been identified in space. The identification of one of the most abundant and widespread interstellar carbenes, the cyclopropenylidene ring, C3H2, is described, together with recent laboratory work on the excited vibrational states of this molecule and on the geometrical structure of one of its isomers, the carbon chain carbene H2C3. A number of additional free carbines which might be detected in space are considered. There are at least two reasons why carbenes are comparatively conspicuous in astronomical sources relative to other reactive molecules: one is their high polarity; a second is their production via the same ion-molecule reactions that make known stable species in space (or very similar reactions). Finally, it is pointed out that cumulene carbon chains somewhat longer than those so far detected in space are promising candidates for the carriers of the interstellar optical diffuse bands.
2

Ziurys, Lucy M. "Interstellar Molecules: The New Frontiers for Molecular Data." In ATOMIC AND MOLECULAR DATA AND THEIR APPLICATIONS: 3rd International Conference on Atomic and Molecular Data and Their Applications ICAMDATA. AIP, 2002. http://dx.doi.org/10.1063/1.1516332.

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3

Gençağa, Deniz, Duane F. Carbon, Kevin H. Knuth, Marcelo de Souza Lauretto, Carlos Alberto de Bragança Pereira, and Julio Michael Stern. "Characterization of Interstellar Organic Molecules." In BAYESIAN INFERENCE AND MAXIMUM ENTROPY METHODS IN SCIENCE AND ENGINEERING: Proceedings of the 28th International Workshop on Bayesian Inference and Maximum Entropy Methods in Science and Engineering. AIP, 2008. http://dx.doi.org/10.1063/1.3039011.

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4

Thimmakondu, Venkatesan. "MOLECULES IN LABORATORY AND IN INTERSTELLAR SPACE?" In 71st International Symposium on Molecular Spectroscopy. Urbana, Illinois: University of Illinois at Urbana-Champaign, 2016. http://dx.doi.org/10.15278/isms.2016.rh05.

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5

Snyder, Lewis E. "Detection of large interstellar molecules with radio interferometers." In Optical Science, Engineering and Instrumentation '97, edited by Richard B. Hoover. SPIE, 1997. http://dx.doi.org/10.1117/12.278783.

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6

Walmsley, C. M. "Ammonia in the interstellar medium." In The 50th international meeting of physical chemistry: Molecules and grains in space. AIP, 1994. http://dx.doi.org/10.1063/1.46570.

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7

Le Bourlot, J., G. Pineau des Fore^ts, E. Roueff, and D. R. Flower. "Atomic carbon in interstellar clouds." In The 50th international meeting of physical chemistry: Molecules and grains in space. AIP, 1994. http://dx.doi.org/10.1063/1.46624.

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8

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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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.
9

Parisel, O., M. Hanus, and Y. Ellinger. "About the formation of interstellar SiN." In The 50th international meeting of physical chemistry: Molecules and grains in space. AIP, 1994. http://dx.doi.org/10.1063/1.46574.

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10

Marty, P., G. Serra, B. Chaudret, and I. Ristorcelli. "Iron-aromatics chemistry in interstellar clouds." In The 50th international meeting of physical chemistry: Molecules and grains in space. AIP, 1994. http://dx.doi.org/10.1063/1.46597.

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Звіти організацій з теми "Interstellar molecules":

1

King, P. K. Gas Dynamics Near and Far: Observational Magnetohydrodynamics of Interstellar Molecular Clouds and X-Ray Ablation of Asteroids for the Earth's Defense. Office of Scientific and Technical Information (OSTI), June 2019. http://dx.doi.org/10.2172/1544929.

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