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Journal articles on the topic 'Interstellar chemistry'

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Published: 4 June 2021
Last updated: 6 September 2023

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1

Seymour, P. A. H. "Interstellar Chemistry." Physics Bulletin 36, no. 7 (July 1985): 305–6. http://dx.doi.org/10.1088/0031-9112/36/7/025.

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2

Klemperer, W. "Interstellar chemistry." Proceedings of the National Academy of Sciences 103, no. 33 (August 7, 2006): 12232–34. http://dx.doi.org/10.1073/pnas.0605352103.

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3

Duley, W. W., D. A. Williams, and Edwin E. Salpeter. "Interstellar Chemistry." Physics Today 38, no. 7 (July 1985): 78–79. http://dx.doi.org/10.1063/1.2814641.

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4

Carbo, R., and A. Ginebreda. "Interstellar chemistry." Journal of Chemical Education 62, no. 10 (October 1985): 832. http://dx.doi.org/10.1021/ed062p832.

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5

RAWLS, REBECCA L. "INTERSTELLAR CHEMISTRY." Chemical & Engineering News Archive 80, no. 28 (July 15, 2002): 31–37. http://dx.doi.org/10.1021/cen-v080n028.p031.

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6

Smith, D. "Interstellar Chemistry." International Journal of Mass Spectrometry and Ion Processes 65, no. 3 (May 1985): 331–32. http://dx.doi.org/10.1016/0168-1176(85)87011-7.

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7

Flower, D. R. "Interstellar chemistry." International Reviews in Physical Chemistry 14, no. 2 (September 1995): 421–43. http://dx.doi.org/10.1080/01442359509353316.

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8

Viti, S., E. Roueff, T. W. Hartquist, G. Pineau des Forêts, and D. A. Williams. "Interstellar oxygen chemistry." Astronomy & Astrophysics 370, no. 2 (May 2001): 557–69. http://dx.doi.org/10.1051/0004-6361:20010246.

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9

Hiraoka, K. "INTERSTELLAR CHEMISTRY: Tunneling Reactions in Interstellar Ices." Science 292, no. 5518 (May 4, 2001): 869–70. http://dx.doi.org/10.1126/science.1060837.

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10

Herbst, E., Q. Chang, and H. M. Cuppen. "Chemistry on interstellar grains." Journal of Physics: Conference Series 6 (January 1, 2005): 18–35. http://dx.doi.org/10.1088/1742-6596/6/1/002.

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11

Hiraoka, Kenzo, Tetsuya Sato, and Toshikazu Takayama. "ChemInform Abstract: Perspectives: Interstellar Chemistry. Tunneling Reactions in Interstellar Ices." ChemInform 32, no. 39 (May 24, 2010): no. http://dx.doi.org/10.1002/chin.200139297.

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12

Goicoechea, J. R., A. Aguado, S. Cuadrado, O. Roncero, J. Pety, E. Bron, A. Fuente, et al. "Bottlenecks to interstellar sulfur chemistry." Astronomy & Astrophysics 647 (March 2021): A10. http://dx.doi.org/10.1051/0004-6361/202039756.

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Hydride molecules lie at the base of interstellar chemistry, but the synthesis of sulfuretted hydrides is poorly understood and their abundances often crudely constrained. Motivated by new observations of the Orion Bar photodissociation region (PDR) – 1″ resolution ALMA images of SH+; IRAM 30 m detections of bright H232S, H234S, and H233S lines; H3S+ (upper limits); and SOFIA/GREAT observations of SH (upper limits) – we perform a systematic study of the chemistry of sulfur-bearing hydrides. We self-consistently determine their column densities using coupled excitation, radiative transfer as well as chemical formation and destruction models. We revise some of the key gas-phase reactions that lead to their chemical synthesis. This includes ab initio quantum calculations of the vibrational-state-dependent reactions SH+ + H2(v) ⇄ H2S+ + H and S + H2 (v) ⇄ SH + H. We find that reactions of UV-pumped H2(v ≥ 2) molecules with S+ ions explain the presence of SH+ in a high thermal-pressure gas component, Pth∕k ≈ 108 cm−3 K, close to the H2 dissociation front (at AV < 2 mag). These PDR layers are characterized by no or very little depletion of elemental sulfur from the gas. However, subsequent hydrogen abstraction reactions of SH+, H2S+, and S atoms with vibrationally excited H2, fail to form enough H2S+, H3S+, and SH to ultimately explain the observed H2S column density (~2.5 × 1014 cm−2, with an ortho-to-para ratio of 2.9 ± 0.3; consistent with the high-temperature statistical value). To overcome these bottlenecks, we build PDR models that include a simple network of grain surface reactions leading to the formation of solid H2S (s-H2S). The higher adsorption binding energies of S and SH suggested by recent studies imply that S atoms adsorb on grains (and form s-H2S) at warmer dust temperatures (Td < 50 K) and closer to the UV-illuminated edges of molecular clouds. We show that everywhere s-H2S mantles form(ed), gas-phase H2S emission lines will be detectable. Photodesorption and, to a lesser extent, chemical desorption, produce roughly the same H2S column density (a few 1014 cm−2) and abundance peak (a few 10−8) nearly independently of nH and G0. This agrees with the observed H2S column density in the Orion Bar as well as at the edges of dark clouds without invoking substantial depletion of elemental sulfur abundances.
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13

Brown, Ronald D., Dinah M. Cragg, and Ryan P. A. Bettens. "Interstellar chemistry: hot-ion reactions." Monthly Notices of the Royal Astronomical Society 245, no. 4 (August 15, 1990): 623. http://dx.doi.org/10.1093/mnras/245.4.623.

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Summary We have explored the possible significance on interstellar chemistry of translationally excited ions (‘hot ions’) produced in exothermic reactions, focusing on weaknesses that remain in existing gas-phase models of cloud chemistry. Particular instances are the lack of success in accounting for observed abundances of NH3, N2H+ and cyanopolyacetylenes. When ‘hot-ion’ reactions are included in the ion-molecule model we obtain predicted abundances in cold clouds like TMC-1, agreeing very well with observations (to better than one order of magnitude) for virtually all smaller molecules included in the model. In particular, the discrepancies for NH3, N2H+ and cyanopolyacetylenes no longer arise. This occurs in the time regime 106.3–106.5 yr [note that this is not the time where the abundance of complex species go through a maximum (˜ 105.5 yr) but somewhat later] and not for very old clouds (age &gt; 107.5 yr). If we use rate constants for hydrogen atom abstraction reactions based on current estimates of their activation energies, then the ‘hot-ion’ reactions do not lead to a noticeable increase in the production of longer chain hydrocarbons. However, for smaller values of these activation energies (for example, those that might make the rate constants around 10−11 cm3 s−1), such hot-ion reactions could dramatically increase the efficiency of carbon-chain building by gas-phase reactions. Therefore, these hot-ion processes may ultimately prove to be the basis of the build-up of these larger species in cold clouds. If the build-up of long chains is to be attributed to the effect of these hot-ion reactions, then the unexpectedly gradual decline in the abundances of CnH, with increasing n, is readily explained. It seems plausible to attribute the irregular variation in these abundances to the enhanced rate of ion-dipolar processes as compared with ion-non-polar reactions, although such influences are more pronounced at greater cloud ages (&gt; 107.5 yr).
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14

Herbst, Eric. "Chemistry in the Interstellar Medium." Annual Review of Physical Chemistry 46, no. 1 (October 1995): 27–54. http://dx.doi.org/10.1146/annurev.pc.46.100195.000331.

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15

Brown, R. D., and E. H. N. Rice. "Galactochemistry – II. Interstellar deuterium chemistry." Monthly Notices of the Royal Astronomical Society 223, no. 2 (November 1986): 429–42. http://dx.doi.org/10.1093/mnras/223.2.429.

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16

Herbst, Eric. "The chemistry of interstellar space." Chemical Society Reviews 30, no. 3 (2001): 168–76. http://dx.doi.org/10.1039/a909040a.

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17

Prasad, Sheo S. "Evolutionary Models of Interstellar Chemistry." Symposium - International Astronomical Union 120 (1987): 259–72. http://dx.doi.org/10.1017/s0074180900154130.

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The goal of evolutionary models of interstellar chemistry is to understand how interstellar clouds came to be the way they are, how they will change with time, and to place them in an evolutionary sequence with other celestial objects such as stars. To this end, we present an improved Mark II version of our earlier model of chemistry in dynamically evolving clouds. The Mark II model suggests that the conventional elemental C/O ratio less than one can explain the observed abundances of CI and the non-detection of O2 in dense clouds. Coupled chemical-dynamical models seem to have the potential to generate many observable discriminators of the evolutionary tracks. This is exciting, because, in general, purely dynamical models do not yield enough verifiable discriminators of the predicted tracks.
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18

Mitchell, George F. "Chemistry in Shocked Interstellar Gas." Symposium - International Astronomical Union 120 (1987): 275–87. http://dx.doi.org/10.1017/s0074180900154154.

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In its passage through the interstellar gas, a shock imposes massive and irreversible changes on the chemical composition of the gas. The synthesis of molecules from atoms and atomic ions can be highly efficient behind non-dissociative (i.e. slow) shocks. Results of kinetic calculations behind non-dissociative shocks are reviewed here, with emphasis given to the dependence of the postshock molecular composition on initial cloud properties. It is shown that a dense cloud shock can convert essentially all neutral atoms into various molecules. Even in diffuse and unshielded regions, a variety of molecules can attain a high abundance behind shocks. The suggestion that the widespread diffuse cloud species CH+ is shock synthesized is critically examined in the light of new calculations.
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19

Prasad, Sheo S. "Evolutionary Models of Interstellar Chemistry." Symposium - International Astronomical Union 150 (1992): 205–10. http://dx.doi.org/10.1017/s0074180900090021.

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Evolutionary chemical models are ultimately unavoidable for a full understanding of interstellar clouds. They include not only the chemical processes but also the dynamical processes by which the modeled object came to be the way it is. From an evolutionary perspective, dark cores may be ephemeral objects and dynamical equilibrium an exception rather than norm. Evolutionary models have numerous advantages over “classical” fixed condition equilibrium models. They have the potential to provide more elegant explanations for the observed inter-cloud and intra-cloud chemical differences. The problem of the depletion of gas phase molecules by condensation onto the grain may also be less serious in evolutionary models. Hence, these models should be actively developed.
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20

Dalgarno, A. "Some problems in interstellar chemistry." International Journal of Mass Spectrometry and Ion Processes 81 (December 1987): 1–13. http://dx.doi.org/10.1016/0168-1176(87)80002-2.

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21

Yamamoto, Satoshi, Hitomi Mikami, and Shuji Saito. "Interstellar Chemistry in Orion KL." International Astronomical Union Colloquium 140 (1994): 190–94. http://dx.doi.org/10.1017/s025292110001945x.

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AbstractA map of SiO (J = 2 − 1) in Ori KL has been obtained with 2.8” spatial resolution by using Nobeyama Millimeter Array. The distribution of SiO evidences an interaction between outflow and dense gas around IRc4 and IRc5; these infrared sources are thus considered to be shock-heated regions. Since distributions of (CH3)2O and HCOOCH3 have a peak at the IRc5 position, such shock heating seems to play an important role in production of these molecules. Detection of CH3OD around the interacting region most likely suggests that CH3OH is evaporating from dust grains. (CH3)2O and HCOOCH3 may be produced by gas-phase reactions starting from injected CH3OH, or they might be evaporated from dust grains.
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22

Charnley, S. B., and A. J. Markwick. "Complex bifurcations in interstellar chemistry?" Astronomy & Astrophysics 399, no. 2 (February 2003): 583–87. http://dx.doi.org/10.1051/0004-6361:20021533.

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23

Langer, William D., and A. E. Glassgold. "Silicon chemistry in interstellar clouds." Astrophysical Journal 352 (March 1990): 123. http://dx.doi.org/10.1086/168519.

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24

Herbst, Eric. "The Chemistry of Interstellar Space." Angewandte Chemie International Edition in English 29, no. 6 (June 1990): 595–608. http://dx.doi.org/10.1002/anie.199005951.

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25

Martinez, Oscar, Theodore P. Snow, and Veronica M. Bierbaum. "Ion chemistry in the interstellar medium." Proceedings of the International Astronomical Union 4, S251 (February 2008): 139–40. http://dx.doi.org/10.1017/s1743921308021388.

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AbstractWithout accurate data on reaction rates and branching ratios, models of interstellar chemistry are unreliable. Recent research has identified a number of reactions of unusual importance because the rates and branching ratios are unknown or poorly known. Efforts to expand and improve on current databases are underway using a flowing afterglow-selected ion flow tube (FA-SIFT) coupled to a quadrupole mass spectrometer. Our current focus is on the reactions of C+, a major cation in the interstellar medium, with the neutrals O2, H2O, CH4, NH3 and C2H2. Future planned work includes studies of polycyclic aromatic hydrocarbons (PAHs), developing comprehensive pathways for their formation, and identification of those PAHs important to interstellar chemistry. The recent discovery of ISM anions has highlighted the importance of examining mechanisms of anionic chemistry in the interstellar medium, and we plan to obtain data relevant to the formation and destruction processes of molecular anions in space.
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26

Jones, A. P. "Dust evolution, a global view I. Nanoparticles, nascence, nitrogen and natural selection … joining the dots." Royal Society Open Science 3, no. 12 (December 2016): 160221. http://dx.doi.org/10.1098/rsos.160221.

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The role and importance of nanoparticles for interstellar chemistry and beyond is explored within the framework of The Heterogeneous dust Evolution Model for Interstellar Solids (THEMIS), focusing on their active surface chemistry, the effects of nitrogen doping and the natural selection of interesting nanoparticle sub-structures. Nanoparticle-driven chemistry, and in particular the role of intrinsic epoxide-type structures, could provide a viable route to the observed gas phase OH in tenuous interstellar clouds en route to becoming molecular clouds. The aromatic-rich moieties present in asphaltenes probably provide a viable model for the structures present within aromatic-rich interstellar carbonaceous grains. The observed doping of such nanoparticle structures with nitrogen, if also prevalent in interstellar dust, could perhaps have important and observable consequences for surface chemistry and the formation of precursor pre-biotic species.
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27

Greenberg, J. Mayo, and Osama M. Shalabiea. "Comets as a Reflection of Interstellar Medium Chemistry." Symposium - International Astronomical Union 160 (1994): 327–42. http://dx.doi.org/10.1017/s0074180900046623.

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A brief summary of the observed infrared and other properties of interstellar dust is given. Chemical, physical and morphological criteria are discussed concerning the degree to which there are constraints relating comets to interstellar dust chemistry representative of the presolar nebula. Results of theoretical modelling of dust and gas evolution in dense clouds are used to compare with observed dust composition. Sources of the distribution of simple as well as complex molecules in the coma are related to what is presently known about the volatile ices in interstellar dust and to processes leading to evaporation of organic “refractory” grain mantle material represented by laboratory residues produced by photoprocessing of ices. The criterion of preservation of interstellar volatiles in comets leads to the further criterion that the ice in comets is amorphous. Criteria for relating interstellar dust volatiles to asteroids are discussed.
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28

Jones, A. P. "Dust evolution, a global view: III. Core/mantle grains, organic nano-globules, comets and surface chemistry." Royal Society Open Science 3, no. 12 (December 2016): 160224. http://dx.doi.org/10.1098/rsos.160224.

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Within the framework of The Heterogeneous dust Evolution Model for Interstellar Solids (THEMIS), this work explores the surface processes and chemistry relating to core/mantle interstellar and cometary grain structures and their influence on the nature of these fascinating particles. It appears that a realistic consideration of the nature and chemical reactivity of interstellar grain surfaces could self-consistently and within a coherent framework explain: the anomalous oxygen depletion, the nature of the CO dark gas, the formation of ‘polar ice’ mantles, the red wing on the 3 μm water ice band, the basis for the O-rich chemistry observed in hot cores, the origin of organic nano-globules and the 3.2 μm ‘carbonyl’ absorption band observed in comet reflectance spectra. It is proposed that the reaction of gas phase species with carbonaceous a-C(:H) grain surfaces in the interstellar medium, in particular the incorporation of atomic oxygen into grain surfaces in epoxide functional groups, is the key to explaining these observations. Thus, the chemistry of cosmic dust is much more intimately related with that of the interstellar gas than has previously been considered. The current models for interstellar gas and dust chemistry will therefore most likely need to be fundamentally modified to include these new grain surface processes.
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29

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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30

Hartquist, T. W. "Chemistry in Shocks." Highlights of Astronomy 8 (1989): 375–82. http://dx.doi.org/10.1017/s1539299600008017.

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ABSTRACTThe column densities of interstellar CH+, first detected about fifty years ago, cannot be explained with models of the chemistry in low temperature gas. The resolution of this classic problem is necessary for us to have confidence in our understanding of interstellar chemistry and its role in determining the physical conditions in interstellar clouds and in the utility of molecular abundance measurements as diagnostics. The possibility that the observed CH+ is formed primarily in shocks in diffuse clouds is addressed. The way in which the chemistry affects the structure of such a diffuse cloud shock is also discussed. The analogous chemical influence on the structures of shocks in dense molecular clouds is also considered as is the possibility that gas in some dense molecular clouds passes repeatedly through dynamical cycles and is shocked frequently enough to influence the global chemical structures in those clouds. Some atomic and molecular data needs are mentioned.
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31

Larsson, Mats. "H3+: the initiator of interstellar chemistry." International Journal of Astrobiology 7, no. 3-4 (August 7, 2008): 237–41. http://dx.doi.org/10.1017/s1473550408004230.

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AbstractSecond only to H2, protonated molecular hydrogen, H3+, is the most abundantly produced interstellar molecule. Owing to its high reactivity and acidity, it plays the pivotal role in initiating interstellar chemical reactions, something which also reduces its steady-state concentration. Interstellar H3+ is not only destroyed in chemical reactions but also in dissociative recombination with electrons. The rate constant and mechanism of recombination have long been controversial, but great advances have been made during recent years, with the important consequence that the cosmic ray ionization rate in diffuse clouds is now believed to be higher by an order of magnitude than previously assumed.
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32

Hartquist, T. W. "Chemistry in Interstellar Hydroxyl Maser Regions." Symposium - International Astronomical Union 120 (1987): 297–302. http://dx.doi.org/10.1017/s0074180900154191.

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The pumping of the upper levels of the 2π3/2 J=3/2 state of OH at sufficient rates to account for the observed strengths of interstellar hydroxyl masers requires that OH contains a substantial fraction of the oxygen. Shocks have been suggested as the sites of the OH production, but a better understanding of OH photodissociation and observations of hydroxyl maser kinematics have led to the realization that the original hydroxyl maser shock model must be revised. the possibility that interstellar hydroxyl masers occur in dense molecular photodissociation zones, heated by photoabsorption and perhaps by ion-neutral friction in the magnetic precursor of a shock, is considered. Possible infrared line emission from interstellar hydroxyl maser regions is mentioned.
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33

Herbst, Eric. "Surface Reactions in Interstellar Space." Highlights of Astronomy 12 (2002): 55–57. http://dx.doi.org/10.1017/s1539299600012818.

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AbstractIt is impossible to explain the abundances of some gas-phase and most condensed-phase interstellar molecules without the use of grain chemistry. Nevertheless, grain-surface chemistry is relatively poorly understood for a variety of reasons. Our current knowledge of this chemistry and its use in interstellar models is discussed along with specific needs for future research.
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34

Williams, David A. "Chemical Effects of Interstellar Grains." Highlights of Astronomy 8 (1989): 383–86. http://dx.doi.org/10.1017/s1539299600008029.

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ABSTRACTThe chemical effects of interstellar grains are briefly reviewed. Their dominant chemical role is to catalyze the formation of H2 which is the seminal molecule for efficient gas phase chemistry. In regions of at least moderate extinction grains accumulate molecular mantles of CO, H2O, etc. Solid state chemistry in such mantles may produce molecules of a type or in an abundance not achievable in the interstellar gas. Return of mantle material to the gas can – at least transiently – dominate gas phase chemistry. It is argued that the freeze-out of heavy atomic and molecular species on to grain surfaces limits the time available for chemistry, restricts molecular cloud chemistry to a “young” character, and suggests that chemical models of molecular clouds must have cyclic dynamics. Such models are briefly described.
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35

Wakelam, V. "Carbon Interstellar Chemistry: Theory versus Observations." Proceedings of the International Astronomical Union 9, S297 (May 2013): 303–10. http://dx.doi.org/10.1017/s1743921313016049.

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AbstractTo study the interstellar chemical composition and interpret molecular observations, astrochemists have built chemical models over the years. Those models compute the composition of the gas and the icy mantles of interstellar grains taking in account a large number of processes, such as chemical reactions in the gas-phase, interactions with grain surfaces (sticking and evaporation) and chemical reactions at the surface of the grains. Those models rely on a number of parameters (physical parameters of the medium and intrinsic chemical parameters such as rate coefficients), which are estimated with an associated uncertainty. From a chemical point of view, those uncertainties are mainly due to an incomplete knowledge of the efficiency of the processes in the interstellar conditions. Many studies in the recent and past years have been undertaken to improve this knowledge, either using experimental or theoretical results in physico-chemistry.
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36

Bron, Emeric, Jacques Le Bourlot, and Franck Le Petit. "Surface chemistry in the interstellar medium." Astronomy & Astrophysics 569 (September 2014): A100. http://dx.doi.org/10.1051/0004-6361/201322101.

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37

Böhme, Diethard Kurt. "Multiply-charged ions and interstellar chemistry." Physical Chemistry Chemical Physics 13, no. 41 (2011): 18253. http://dx.doi.org/10.1039/c1cp21814j.

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38

Wiesemeyer, H., R. Güsten, K. M. Menten, C. A. Durán, T. Csengeri, A. M. Jacob, R. Simon, J. Stutzki, and F. Wyrowski. "Unveiling the chemistry of interstellar CH." Astronomy & Astrophysics 612 (April 2018): A37. http://dx.doi.org/10.1051/0004-6361/201731810.

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Context. The methylidyne radical CH is commonly used as a proxy for molecular hydrogen in the cold, neutral phase of the interstellar medium. The optical spectroscopy of CH is limited by interstellar extinction, whereas far-infrared observations provide an integral view through the Galaxy. While the HF ground state absorption, another H2 proxy in diffuse gas, frequently suffers from saturation, CH remains transparent both in spiral-arm crossings and high-mass star forming regions, turning this light hydride into a universal surrogate for H2. However, in slow shocks and in regions dissipating turbulence its abundance is expected to be enhanced by an endothermic production path, and the idea of a “canonical” CH abundance needs to be addressed. Aim. The N = 2 ← 1 ground state transition of CH at λ149 μm has become accessible to high-resolution spectroscopy thanks to the German Receiver for Astronomy at Terahertz Frequencies (GREAT) aboard the Stratospheric Observatory for Infrared Astronomy (SOFIA). Its unsaturated absorption and the absence of emission from the star forming regions makes it an ideal candidate for the determination of column densities with a minimum of assumptions. Here we present an analysis of four sightlines towards distant Galactic star forming regions, whose hot cores emit a strong far-infrared dust continuum serving as background signal. Moreover, if combined with the sub-millimeter line of CH at λ560 μm , environments forming massive stars can be analyzed. For this we present a case study on the “proto-Trapezium” cluster W3 IRS5. Methods. While we confirm the global correlation between the column densities of HF and those of CH, both in arm and interarm regions, clear signposts of an over-abundance of CH are observed towards lower densities. However, a significant correlation between the column densities of CH and HF remains. A characterization of the hot cores in the W3 IRS5 proto-cluster and its envelope demonstrates that the sub-millimeter/far-infrared lines of CH reliably trace not only diffuse but also dense, molecular gas. Results. In diffuse gas, at lower densities a quiescent ion-neutral chemistry alone cannot account for the observed abundance of CH. Unlike the production of HF, for CH+ and CH, vortices forming in turbulent, diffuse gas may be the setting for an enhanced production path. However, CH remains a valuable tracer for molecular gas in environments reaching from diffuse clouds to sites of high-mass star formation.
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39

Le Bourlot, J., F. Le Petit, C. Pinto, E. Roueff, and F. Roy. "Surface chemistry in the interstellar medium." Astronomy & Astrophysics 541 (May 2012): A76. http://dx.doi.org/10.1051/0004-6361/201118126.

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40

Boger, Gai I., and Amiel Sternberg. "Bistability in Interstellar Gas‐Phase Chemistry." Astrophysical Journal 645, no. 1 (July 2006): 314–23. http://dx.doi.org/10.1086/502624.

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41

Klotz, A., and B. Chaudret. "Organometallic Chemistry in the interstellar medium." EAS Publications Series 4 (2002): 55. http://dx.doi.org/10.1051/eas:2002059.

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42

Snow, Theodore P., and Veronica M. Bierbaum. "Ion Chemistry in the Interstellar Medium." Annual Review of Analytical Chemistry 1, no. 1 (July 2008): 229–59. http://dx.doi.org/10.1146/annurev.anchem.1.031207.112907.

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43

Mandal, Swadhin K., and Herbert W. Roesky. "Interstellar molecules: guides for new chemistry." Chemical Communications 46, no. 33 (2010): 6016. http://dx.doi.org/10.1039/c0cc01003k.

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44

Roueff, Evelyne, and Jacques Le Bourlot. "Sustained oscillations in interstellar chemistry models." Astronomy & Astrophysics 643 (November 2020): A121. http://dx.doi.org/10.1051/0004-6361/202039085.

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Context. Nonlinear behavior in interstellar chemical models has been recognized for 25 years now. Different mechanisms account for the possibility of multiple fixed-points at steady-state, characterized by the ionization degree of the gas. Aims. Chemical oscillations are also a natural behavior of nonlinear chemical models. We study under which conditions spontaneous sustained chemical oscillations are possible, and what kind of bifurcations lead to, or quench, the occurrence of such oscillations. Methods. The well-known ordinary differential equations (ODE) integrator VODE was used to explore initial conditions and parameter space in a gas phase chemical model of a dark interstellar cloud. Results. We recall that the time evolution of the various chemical abundances under fixed temperature conditions depends on the density over cosmic ionization rate nH∕ζ ratio. We also report the occurrence of naturally sustained oscillations for a limited but well-defined range of control parameters. The period of oscillations is within the range of characteristic timescales of interstellar processes and could lead to spectacular resonances in time-dependent models. Reservoir species (C, CO, NH3, ...) oscillation amplitudes are generally less than a factor two. However, these amplitudes reach a factor ten to thousand for low abundance species, e.g. HCN, ND3, that may play a key role for diagnostic purposes. The mechanism responsible for oscillations is tightly linked to the chemistry of nitrogen, and requires long chains of reactions such as found in multi-deuteration processes.
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45

Spaans, Marco. "Interstellar Chemistry: Radiation, Dust and Metals." Proceedings of the International Astronomical Union 4, S255 (June 2008): 238–45. http://dx.doi.org/10.1017/s1743921308024885.

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AbstractAn overview is given of the chemical processes that occur in primordial systems under the influence of radiation, metal abundances and dust surface reactions. It is found that radiative feedback effects differ for UV and X-ray photons at any metallicity, with molecules surviving quite well under irradiation by X-rays. Starburst and AGN will therefore enjoy quite different cooling abilities for their dense molecular gas. The presence of a cool molecular phase is strongly dependent on metallicity. Strong irradiation by cosmic rays (>200× the Milky Way value) forces a large fraction of the CO gas into neutral carbon. Dust is important for H2 and HD formation, already at metallicities of 10−4 − 10−3 solar, for electron abundances below 10−3.
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46

Langer, William D., and T. E. Graedel. "The Nitrogen Chemistry in Interstellar Clouds." Symposium - International Astronomical Union 120 (1987): 305–10. http://dx.doi.org/10.1017/s007418090015421x.

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Our time dependent model of chemistry of dense interstellar clouds has been extended to study the formation of nitrogen bearing molecules. Here we present results for the calculations, under a variety of density, temperature, and elemental conditions, of the abundances of the following observationally important species: CN, HCN, HNC, NH3, NO, and N2H.
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47

Snow, Theodore P., Valery Le Page, Yeghis Keheyan, and Veronica M. Bierbaum. "The interstellar chemistry of PAH cations." Nature 391, no. 6664 (January 1998): 259–60. http://dx.doi.org/10.1038/34602.

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48

Smith, David. "The ion chemistry of interstellar clouds." Chemical Reviews 92, no. 7 (November 1992): 1473–85. http://dx.doi.org/10.1021/cr00015a001.

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49

Charnley, S. B. "The interstellar chemistry of protostellar disks." Astrophysics and Space Science 224, no. 1-2 (February 1995): 441–42. http://dx.doi.org/10.1007/bf00667895.

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50

Loison, Jean-Christophe, Marcelino Agúndez, Núria Marcelino, Valentine Wakelam, Kevin M. Hickson, José Cernicharo, Maryvonne Gerin, Evelyne Roueff, and Michel Guélin. "The interstellar chemistry of H2C3O isomers." Monthly Notices of the Royal Astronomical Society 456, no. 4 (January 22, 2016): 4101–10. http://dx.doi.org/10.1093/mnras/stv2866.

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