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

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

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1

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

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Abstract Enols—tautomers of ketones or aldehydes—are considered key intermediates in the formation of prebiotic sugars and sugar acids. Although laboratory simulation experiments suggest that enols should be ubiquitous in the interstellar medium, the underlying formation mechanisms of enols in interstellar environments are largely elusive. Here, we present the laboratory experiments on the formation of glyoxal (HCOCHO) along with its ynol tautomer acetylenediol (HOCCOH) in interstellar ice analogs composed of carbon monoxide (CO) and water (H2O) upon exposure to energetic electrons as a proxy
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2

Wang, Jia, Chaojiang Zhang, Joshua H. Marks, and Ralf I. Kaiser. "Formation of All Three C2H4O Isomers—Ethylene Oxide (c-C2H4O), Acetaldehyde (CH3CHO), and Vinyl Alcohol (CH2CHOH)—in Ethanol-containing Interstellar Analog Ices." Astrophysical Journal 984, no. 2 (2025): 138. https://doi.org/10.3847/1538-4357/adc308.

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Abstract Oxygen-containing complex organic molecules are key precursors to biorelevant compounds fundamental for the origins of life. However, the untangling of their interstellar formation mechanisms has just scratched the surface, especially for oxygen-containing cyclic molecules. Here, we present the first laboratory simulation experiments featuring the formation of all three C2H4O isomers—ethylene oxide (c–C2H4O), acetaldehyde (CH3CHO), and vinyl alcohol (CH2CHOH)—in low-temperature model interstellar ices composed of carbon monoxide (CO) and ethanol (C2H5OH). Ice mixtures were exposed to
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3

Abplanalp, Matthew J., and Ralf I. Kaiser. "On the formation of complex organic molecules in the interstellar medium: untangling the chemical complexity of carbon monoxide–hydrocarbon containing ice analogues exposed to ionizing radiation via a combined infrared and reflectron time-of-flight analysis." Physical Chemistry Chemical Physics 21, no. 31 (2019): 16949–80. http://dx.doi.org/10.1039/c9cp01793c.

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4

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

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A novel mechanism is proposed for the electron-induced production of methyl formate from CO and CH<sub>3</sub>OH which is relevant for interstellar ice chemistry. A key-step in this reaction is the formation of an intermediate CH<sub>3</sub>OCO radical.
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5

Kuznetsov, O. V., M. M. Evseev, E. A. Batrakova, and I. O. Antonov. "Ionization Energy of Reaction Products in an Ethanol–Carbon Monoxide System in Interstellar Ices." Bulletin of the Lebedev Physics Institute 51, no. 3 (2024): 77–82. http://dx.doi.org/10.3103/s1068335623601826.

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6

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

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AbstractWe present experimental studies on the interaction of heavy, highly charged and energetic ions (46 MeV 58Ni13+) with interstellar ammonia-containing (H2O:NH3:CO) ice analog in an attempt to simulate the physical chemistry induced by heavy ion cosmic rays inside dense astrophysical environments. The measurements were performed at the heavy ion accelerator GANIL in Caen, France. In-situ analysis have been performed by a Fourier transform infrared spectrometer. The averaged values for the dissociation cross section of water, ammonia and carbon monoxide are determined and the estimated hal
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7

Bennett, Chris J., Corey S. Jamieson, and Ralf I. Kaiser. "AN EXPERIMENTAL INVESTIGATION OF THE DECOMPOSITION OF CARBON MONOXIDE AND FORMATION ROUTES TO CARBON DIOXIDE IN INTERSTELLAR ICES." Astrophysical Journal Supplement Series 182, no. 1 (2009): 1–11. http://dx.doi.org/10.1088/0067-0049/182/1/1.

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8

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

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A fundamental problem in astrochemistry concerns the synthesis and survival of complex organic molecules (COMs) throughout the process of star and planet formation. While it is generally accepted that most complex molecules and prebiotic species form in the solid phase on icy grain particles, a complete understanding of the formation pathways is still largely lacking. To take full advantage of the enormous number of available THz observations (e.g.,Herschel Space Observatory, SOFIA, and ALMA), laboratory analogs must be studied systematically. Here, we present the THz (0.3–7.5 THz; 10–250 cm<s
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9

Collings, M. P., J. W. Dever, M. R. S. McCoustra, and H. J. Fraser. "Implications of Ice Morphology for Comet Formation." Highlights of Astronomy 13 (2005): 491–94. http://dx.doi.org/10.1017/s1539299600016397.

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AbstractLaboratory surface science under ultra-high vacuum (UHV) conditions allows us to simulate the growth of ices in astrophysical environments. Using the techniques of temperature programmed desorption (TPD), reflection-absorption infrared spectroscopy (RAIRS) and micro-balance methods, we have studied binary ice systems consisting of water (H2O) and variety of other species including carbon monoxide (CO), at astrophysically relevant conditions of temperature and pressure. We present results that demonstrate that the morphology of water ice has an important influence on the behavior of suc
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10

Huang, C. H., A. Ciaravella, C. Cecchi-Pestellini, et al. "Effects of 150–1000 eV Electron Impacts on Pure Carbon Monoxide Ices Using the Interstellar Energetic-Process System (IEPS)." Astrophysical Journal 889, no. 1 (2020): 57. http://dx.doi.org/10.3847/1538-4357/ab5dbe.

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11

Hasegawa, Takeshi, Hiroto Yanagisawa, Takumi Nagasawa, Reo Sato, Naoki Numadate, and Tetsuya Hama. "Infrared Band Strengths of Dangling OH Features in Amorphous Water at 20 K." Astrophysical Journal 969, no. 2 (2024): 134. http://dx.doi.org/10.3847/1538-4357/ad5318.

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Abstract Infrared (IR) spectra of vapor-deposited amorphous water at low temperatures show two weak peaks at around 3720 and 3696 cm−1 assigned to free-OH stretching modes of two- and three-coordinated water molecules (so-called “dangling” OH bonds), respectively, on the ice surface. A recent JWST observation first succeeded in detection of a potential dangling OH feature at 3664 cm−1 for ices in molecular clouds, highlighting the importance of dangling OH bonds in interstellar ice chemistry. A lack of band strengths of these features at low temperatures restricts the quantification of danglin
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12

Turner, Andrew M., Alexandre Bergantini, Andreas S. Koutsogiannis, et al. "A Photoionization Mass Spectrometry Investigation into Complex Organic Molecules Formed in Interstellar Analog Ices of Carbon Monoxide and Water Exposed to Ionizing Radiation." Astrophysical Journal 916, no. 2 (2021): 74. http://dx.doi.org/10.3847/1538-4357/ac0537.

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13

Maity, Surajit, Ralf I. Kaiser, and Brant M. Jones. "FORMATION OF KETENE (H2CCO) IN INTERSTELLAR ANALOGOUS METHANE (CH4)-CARBON MONOXIDE (CO) ICES: A COMBINED FTIR AND REFLECTRON TIME-OF-FLIGHT MASS SPECTROSCOPIC STUDY." Astrophysical Journal 789, no. 1 (2014): 36. http://dx.doi.org/10.1088/0004-637x/789/1/36.

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14

Hudson, R. L., and M. H. Moore. "Laboratory Studies of the Formation of Methanol and Other Organic Molecules by Water+Carbon Monoxide Radiolysis: Relevance to Comets, Icy Satellites, and Interstellar Ices." Icarus 140, no. 2 (1999): 451–61. http://dx.doi.org/10.1006/icar.1999.6144.

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15

Lambert, David L., Yaron Sheffer, Ronald L. Gilliland, and S. R. Federman. "Interstellar carbon monoxide toward zeta Ophiuchi." Astrophysical Journal 420 (January 1994): 756. http://dx.doi.org/10.1086/173600.

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16

Crenny, T., and S. R. Federman. "Reanalysis ofCopernicusMeasurements of Interstellar Carbon Monoxide." Astrophysical Journal 605, no. 1 (2004): 278–84. http://dx.doi.org/10.1086/382231.

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17

M. Wallace, Austin, and Ryan C. Fortenberry. "Computational UV spectra for amorphous solids of small molecules." Physical Chemistry Chemical Physics 23, no. 42 (2021): 24413–20. http://dx.doi.org/10.1039/d1cp03255k.

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18

Lamberts, T. "From interstellar carbon monosulfide to methyl mercaptan: paths of least resistance." Astronomy & Astrophysics 615 (July 2018): L2. http://dx.doi.org/10.1051/0004-6361/201832830.

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The 29 reactions linking carbon monosulfide (CS) to methyl mercaptan (CH3SH) via ten intermediate radicals and molecules have been characterized with relevance to surface chemistry in cold interstellar ices. More intermediate species than previously considered are found likely to be present in these ices, such as trans- and cis-HCSH. Both activation and reaction energies have been calculated, along with low-temperature (T &gt; 45 K) rate constants for the radical-neutral reactions. For barrierless radical-radical reactions on the other hand, branching ratios have been determined. The combinati
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19

Marks, Joshua H., Jia Wang, Mikhail M. Evseev, Oleg V. Kuznetsov, Ivan O. Antonov, and Ralf I. Kaiser. "Complex Reactive Acids from Methanol and Carbon Dioxide Ice: Glycolic Acid (HOCH2COOH) and Carbonic Acid Monomethyl Ester (CH3OCOOH)." Astrophysical Journal 942, no. 1 (2023): 43. http://dx.doi.org/10.3847/1538-4357/ac97e3.

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Abstract The formation of complex organic molecules by simulated secondary electrons generated in the track of galactic cosmic rays was investigated in interstellar ice analogs composed of methanol and carbon dioxide. The processed ices were subjected to temperature-programmed desorption to mimic the transition of a cold molecular cloud to a warmer star-forming region. Reaction products were detected as they sublime using photoionization reflectron time-of-flight mass spectrometry. By employing isotopic labeling, tunable photoionization and computed adiabatic ionization energies isomers of C2H
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20

Collings, M. P., J. W. Dever, H. J. Fraser, M. R. S. McCoustra, and D. A. Williams. "Carbon Monoxide Entrapment in Interstellar Ice Analogs." Astrophysical Journal 583, no. 2 (2003): 1058–62. http://dx.doi.org/10.1086/345389.

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21

Whittet, D. C. B., and W. W. Duley. "Carbon monoxide frosts in the interstellar medium." Astronomy and Astrophysics Review 2, no. 3-4 (1991): 167–89. http://dx.doi.org/10.1007/bf00872766.

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22

Ehrenfreund, Pascale, and Oliver Botta. "From Interstellar Matter To Comets: A Laboratory View." Highlights of Astronomy 13 (2005): 488–90. http://dx.doi.org/10.1017/s1539299600016385.

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AbstractComets, formed in the cold outer parts of the solar system, provide a record of pristine material from the parent interstellar cloud. The investigation of outgassing curves from bright comets has provided a relationship to the abundances of interstellar ices and gas phase molecules. However, being porous and stratified in various layers of different densities and temperatures, the out-gassing characteristics of comets can not always be directly reconciled with the interstellar composition. This is due to the structure of the nuclear ice component, which contains different coexisting ic
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23

Arshutkin, L. N. "Study of carbon monoxide formation in interstellar clouds." Astrophysics 22, no. 1 (1985): 100–107. http://dx.doi.org/10.1007/bf01084466.

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24

Bodewits, D., J. W. Noonan, P. D. Feldman, et al. "The carbon monoxide-rich interstellar comet 2I/Borisov." Nature Astronomy 4, no. 9 (2020): 867–71. http://dx.doi.org/10.1038/s41550-020-1095-2.

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25

Allamandola, Louis J., Max P. Bernstein, and Scott A. Sandford. "Photochemical Evolution of Interstellar/Precometary Organic Material." International Astronomical Union Colloquium 161 (January 1997): 23–47. http://dx.doi.org/10.1017/s0252921100014585.

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AbstractInfrared observations, combined with realistic laboratory simulations, have revolutionized our understanding of interstellar ice and dust, the building blocks of comets. Since comets are thought to be a major source of the volatiles on the primative earth, their organic inventory is of central importance to questions concerning the origin of life. Ices in molecular clouds contain the very simple molecules H2O, CH3OH, CO, CO2, CH4, H2, and probably some NH3and H2CO, as well as more complex species including nitriles, ketones, and esters. The evidence for these, as well as carbonrich mat
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26

Maity, Surajit, Ralf I. Kaiser, and Brant M. Jones. "Formation of complex organic molecules in methanol and methanol–carbon monoxide ices exposed to ionizing radiation – a combined FTIR and reflectron time-of-flight mass spectrometry study." Physical Chemistry Chemical Physics 17, no. 5 (2015): 3081–114. http://dx.doi.org/10.1039/c4cp04149f.

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The radiation induced chemical processing of methanol and methanol–carbon monoxide ices at 5.5 K exposed to ionizing radiation in the form of energetic electrons and subsequent temperature programmed desorption is reported in this study.
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27

Mifsud, Duncan V., Péter Herczku, Béla Sulik, et al. "Proton and Electron Irradiations of CH4:H2O Mixed Ices." Atoms 11, no. 2 (2023): 19. http://dx.doi.org/10.3390/atoms11020019.

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The organic chemistry occurring in interstellar environments may lead to the production of complex molecules that are relevant to the emergence of life. Therefore, in order to understand the origins of life itself, it is necessary to probe the chemistry of carbon-bearing molecules under conditions that simulate interstellar space. Several of these regions, such as dense molecular cores, are exposed to ionizing radiation in the form of galactic cosmic rays, which may act as an important driver of molecular destruction and synthesis. In this paper, we report the results of a comparative and syst
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28

Federman, S. R., Jason A. Cardelli, Yaron Sheffer, David L. Lambert, and D. C. Morton. "Intersystem transitions of interstellar carbon monoxide toward zeta Ophiuchi." Astrophysical Journal 432 (September 1994): L139. http://dx.doi.org/10.1086/187531.

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29

Zhang, Chaojiang, Leslie A. Young, and Ralf I. Kaiser. "Chemical Evolution of Isotopically Labeled Carbon Dioxide (13CO2) Ice Exposed to Ionizing Radiation and Implications for Trans-Neptunian Objects." Astrophysical Journal 980, no. 2 (2025): 248. https://doi.org/10.3847/1538-4357/ada9e7.

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Abstract We present results on the radiation chemistry of isotopically labeled carbon dioxide (13CO2) ices induced by energetic electrons at 40 and 10 K to simulate the chemical evolution of carbon dioxide on trans-Neptunian objects exposed to galactic cosmic-ray particles. By collecting infrared spectra during the irradiation of 13CO2 ices, we have identified several radiolysis products, including carbon monoxide (13CO), ozone (O3), carbon trioxide (13CO3) with cyclic (C 2v ) and acyclic (D 3h ) isomers, carbon tetraoxide (13CO4), carbon pentaoxide (13CO5), and carbon hexaoxide (13CO6). The t
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30

Maity, Surajit, and Ralf I. Kaiser. "ELECTRON IRRADIATION OF CARBON DISULFIDE-OXYGEN ICES: TOWARD THE FORMATION OF SULFUR-BEARING MOLECULES IN INTERSTELLAR ICES." Astrophysical Journal 773, no. 2 (2013): 184. http://dx.doi.org/10.1088/0004-637x/773/2/184.

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31

Bergin, Edwin A., Arthur Bosman, Richard Teague, et al. "The Carbon Isotopic Ratio and Planet Formation." Astrophysical Journal 965, no. 2 (2024): 147. http://dx.doi.org/10.3847/1538-4357/ad3443.

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Abstract We present the first detection of 13CCH in a protoplanetary disk (TW Hya). Using observations of C2H, we measure CCH/13CCH = 65 ± 20 gas with a CO isotopic ratio of 12CO/13CO = 21 ± 5. The TW Hya disk exhibits a gas phase C/O that exceeds unity, and C2H is the tracer of this excess carbon. We confirm that the TW Hya gaseous disk exhibits two separate carbon isotopic reservoirs, as noted previously. We explore two theoretical solutions for the development of this dichotomy. One model represents TW Hya today with a protoplanetary disk exposed to a cosmic-ray ionization rate that is belo
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32

Qasim, D., M. J. A. Witlox, G. Fedoseev, et al. "A cryogenic ice setup to simulate carbon atom reactions in interstellar ices." Review of Scientific Instruments 91, no. 5 (2020): 054501. http://dx.doi.org/10.1063/5.0003692.

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33

Israel, F. P., and Th De Graauw. "Carbon Monoxide in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 45–49. http://dx.doi.org/10.1017/s007418090019998x.

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Molecular gas is a major constituent of the interstellar medium of all late-type galaxies. Virtually all of it is in the form of cold molecular hydrogen (H2) which today cannot be observed directly. However, the tracer molecule carbon monoxide (CO) (relative abundance 10−5) is easily detected. For the Magellanic Clouds (MCs), CO studies are of specific importance. The Clouds are rich in HI, and if we can establish the presence of significant amounts of H2 as well, this will influence our estimates of the global rate of star formation and its history. Complexes of presently quiescent molecular
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34

Roser, Joe E., Gianfranco Vidali, Giulio Manicò, and Valerio Pirronello. "Formation of Carbon Dioxide by Surface Reactions on Ices in the Interstellar Medium." Astrophysical Journal 555, no. 1 (2001): L61—L64. http://dx.doi.org/10.1086/321732.

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35

Ahrens, Caitlin, Hypatia Meraviglia, and Christopher Bennett. "A Geoscientific Review on CO and CO2 Ices in the Outer Solar System." Geosciences 12, no. 2 (2022): 51. http://dx.doi.org/10.3390/geosciences12020051.

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Ground-based telescopes and space exploration have provided outstanding observations of the complexity of icy planetary surfaces. This work presents our review of the varying nature of carbon dioxide (CO2) and carbon monoxide (CO) ices from the cold traps on the Moon to Pluto in the Kuiper Belt. This review is organized into five parts. First, we review the mineral physics (e.g., rheology) relevant to these environments. Next, we review the radiation-induced chemical processes and the current interpretation of spectral signatures. The third section discusses the nature and distribution of CO2
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36

Ferrero, Stefano, Cecilia Ceccarelli, Piero Ugliengo, Mariona Sodupe, and Albert Rimola. "Formation of Interstellar Complex Organic Molecules on Water-rich Ices Triggered by Atomic Carbon Freezing." Astrophysical Journal 960, no. 1 (2023): 22. http://dx.doi.org/10.3847/1538-4357/ad0547.

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Abstract The reactivity of interstellar carbon atoms (C) on water-dominated ices is one of the possible ways to form interstellar complex organic molecules (iCOMs). In this work, we report a quantum chemical study of the coupling reaction of C (3P) with an icy water molecule, alongside possible subsequent reactions with the most abundant closed-shell frozen species (NH3, CO, CO2, and H2), atoms (H, N, and O), and molecular radicals (OH, NH2, and CH3). We found that C reacts spontaneously with the water molecule, resulting in the formation of 3C–OH2, a highly reactive species due to its triplet
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37

Whittet, D. C. B. "Interstellar Dust and the Organic Inventories of Early Solar Systems." Symposium - International Astronomical Union 213 (2004): 163–68. http://dx.doi.org/10.1017/s0074180900193192.

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Interstellar dust grains are vectors for cosmic carbon and other biogenic chemical elements. They deliver carbon to protoplanetary disks in various refractory phases (amorphous, graphitic, etc.), and they are coated with icy mantles that contain organic molecules and water. The nature of the organics present in and on the dust appears to be closely related to physical conditions. Complex molecules may be synthesized when simple ices are irradiated. Astronomical observations show that this occurs in the vicinity of certain massive protostars, but it is not known whether our Solar System formed
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38

Zamirri, Lorenzo, Silvia Casassa, Albert Rimola, Mireia Segado-Centellas, Cecilia Ceccarelli, and Piero Ugliengo. "IR spectral fingerprint of carbon monoxide in interstellar water–ice models." Monthly Notices of the Royal Astronomical Society 480, no. 2 (2018): 1427–44. http://dx.doi.org/10.1093/mnras/sty1927.

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39

Ciaravella, A., A. Jiménez-Escobar, G. M. Muñoz Caro, et al. "SOFT X-RAY IRRADIATION OF PURE CARBON MONOXIDE INTERSTELLAR ICE ANALOGUES." Astrophysical Journal 746, no. 1 (2012): L1. http://dx.doi.org/10.1088/2041-8205/746/1/l1.

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40

Shingledecker, C. N., K. L. K. Lee, J. T. Wandishin, et al. "Detection of interstellar H2CCCHC3N." Astronomy & Astrophysics 652 (August 2021): L12. http://dx.doi.org/10.1051/0004-6361/202140698.

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Context. The chemical pathways linking the small organic molecules commonly observed in molecular clouds to the large, complex, polycyclic species long suspected of being carriers of the ubiquitous unidentified infrared emission bands remain unclear. Aims. To investigate whether the formation of mono- and polycyclic molecules observed in cold cores could form via the bottom-up reaction of ubiquitous carbon-chain species with, for example, atomic hydrogen, a search is made for possible intermediates in data taken as part of the GOTHAM (GBT Observations of TMC-1: Hunting for Aromatic Molecules)
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41

Ferrero, Stefano, Cecilia Ceccarelli, Piero Ugliengo, Mariona Sodupe, and Albert Rimola. "Formation of Complex Organic Molecules on Interstellar CO Ices? Insights from Computational Chemistry Simulations." Astrophysical Journal 951, no. 2 (2023): 150. http://dx.doi.org/10.3847/1538-4357/acd192.

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Abstract The carbon (3P) atom is a reactive species that, according to laboratory experiments and theoretical calculations, condensates with interstellar ice components. This fact is of uttermost importance for the chemistry in the interstellar medium (ISM) because the condensation reaction is barrierless, and the subsequent species formed are still reactive given their open-shell character. Carbon condensation on CO-rich ices forms the C=C=O (3Σ−) species, which can be easily hydrogenated twice to form ketene (H2CCO). Ketene is very reactive in terrestrial conditions, usually found as an inte
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42

Sivaraman, Bhalamurugan, Sohan Jheeta, Nigel Mason, et al. "Electron, proton and ion induced molecular synthesis and VUV spectroscopy of interstellar molecules in the ice phase." Proceedings of the International Astronomical Union 4, S251 (2008): 451–52. http://dx.doi.org/10.1017/s1743921308022163.

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AbstractPlanets and their moons are constantly subjected to irradiation from both their respective planetary magnetospheres and the solar wind. Energetic particles (electrons, protons and ions) in such radiation may induce complex chemistry within the icy mantles of such bodies, producing many organic compounds. Such processes can be simulated in laboratory experiments. In this report we present recent results from experiments exploring both molecular synthesis and the morphology of such ices.The morphology of any ice may be characterised by IR and Vacuum Ultra-Violet (VUV) spectroscopy. The l
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43

Kalvāns, Juris, and Juris Roberts Kalnin. "Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains." Astrophysical Journal Supplement Series 263, no. 1 (2022): 5. http://dx.doi.org/10.3847/1538-4365/ac92e6.

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Abstract Icy grains in the interstellar medium and star formation regions consist of a variety of materials. Such composite grains interact differently with cosmic-ray (CR) particles compared to simple single-material grains. We aim to calculate the spectra of energies and temperatures of mixed-composition grains undergoing whole-grain heating by CRs. The grains were assumed to consist of a mixture of carbon and olivine, covered by ices consisting of carbon oxides and water. The energy and temperature spectra for grains with radii 0.05, 0.1, and 0.2 μm impacted by CRs were calculated for eight
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44

Luna, Ramón, Carlos Millán, Manuel Domingo, Carmina Santonja, and Miguel Á. Satorre. "Density and Refractive Index of Carbon Monoxide Ice at Different Temperatures." Astrophysical Journal 935, no. 2 (2022): 134. http://dx.doi.org/10.3847/1538-4357/ac8001.

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Abstract This paper is intended to study the density and the refractive index of the solid carbon monoxide in the interval 13–28 K to improve our understanding of the dynamics in the astrophysical environments where they are present. A series of deposition experiments have been performed under high vacuum conditions to study the properties of this ice under astrophysical conditions. Ice density has been experimentally calculated at different deposition temperatures of astrophysical interest, which complement the scarce values present in the literature. The refractive index has also been experi
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45

Taj, S., and M. R. S. McCoustra. "Thermal desorption of carbon monoxide from model interstellar ice surfaces: revealing surface heterogeneity." Monthly Notices of the Royal Astronomical Society 498, no. 2 (2020): 1693–99. http://dx.doi.org/10.1093/mnras/staa2372.

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ABSTRACT Temperature programmed desorption has been used to probe the distribution of binding energies of carbon monoxide (CO) to molecular solid thin films of astrophysical relevance. Measurements are reported for solid water (both compact amorphous solid water and crystalline water), ammonia, and methanol surfaces. Binding energy distributions and optimized pre-exponential factors based on the inversion method are tabulated. These are compared to existing data on these systems and astrophysical conclusions drawn.
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46

Neufeld, David A. "COLLISIONAL EXCITATION OF FAR-INFRARED LINE EMISSIONS FROM WARM INTERSTELLAR CARBON MONOXIDE (CO)." Astrophysical Journal 749, no. 2 (2012): 125. http://dx.doi.org/10.1088/0004-637x/749/2/125.

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47

Keller, L. P., K. L. Thomas, J. P. Bradley, and D. E. Brownlee. "Quantitative analyses of total carbon in interplanetary dust particles." Proceedings, annual meeting, Electron Microscopy Society of America 50, no. 2 (1992): 1724–25. http://dx.doi.org/10.1017/s0424820100133254.

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Interplanetary dust particles (IDPs) collected in the stratosphere are believed to be derived from comets and asteroids. The abundance and chemical state of carbon in IDPs are of particular importance because they provide insight into the processes that have affected carbon from its nucleosynthesis to its incorporation into primitive solar system bodies. Sources of carbon in IDPs may include primary circumstellar condensates (e.g. SiC and graphitic carbons), organic phases derived from the interstellar medium (e.g. polycyclic aromatic hydrocarbons and other residues from radiation-processed ic
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48

Spaans, M. "The Structure of the Multi-Phase ISM in Low Surface Brightness Galaxies." International Astronomical Union Colloquium 171 (1999): 237–44. http://dx.doi.org/10.1017/s0252921100054397.

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AbstractThe multi-phase structure of the interstellar medium in low surface brightness galaxies is investigated and compared to observations. It is found that the ambient pressure and metallicity very strongly influence the abundances of molecular hydrogen and carbon monoxide. The emissivity of the latter is computed and found to agree naturally with the upper limits measured for low surface brightness galaxies. The implications for star formation efficiency and galaxy evolution are discussed.
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49

Dartois, E., M. Chabot, T. Id Barkach, et al. "Cosmic ray sputtering yield of interstellar ice mantles." Astronomy & Astrophysics 647 (March 2021): A177. http://dx.doi.org/10.1051/0004-6361/202039535.

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Aims. Cosmic-ray-induced sputtering is one of the important desorption mechanisms at work in astrophysical environments. The chemical evolution observed in high-density regions, from dense clouds to protoplanetary disks, and the release of species condensed on dust grains, is one key parameter to be taken into account in interpretations of both observations and models. Methods. This study is part of an ongoing systematic experimental determination of the parameters to consider in astrophysical cosmic ray sputtering. As was already done for water ice, we investigated the sputtering yield as a f
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50

Andreani, Paola, Lazaros Souvaitzis, Padelis Papadopoulos, et al. "The Interstellar and Circumgalactic Media at low and high redshift as traced by Atomic Carbon and Carbon Monoxide." EPJ Web of Conferences 265 (2022): 00046. http://dx.doi.org/10.1051/epjconf/202226500046.

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A different chemistry of the interstellar medium (ISM) is expected in the circumgalactic medium (CGM) gas where high-energetic particles (i.e. cosmic rays) seem to be produced in-situ by the hot X-ray gas, as it is observed in the Perseus cluster. This very different astrochemistry, where extreme gas-dust thermal decoupling is expected, and where CO can be destroyed over large massscales, is the subject of the investigation briefly reported here. We introduce an on-going project aiming at studying the properties of the CGM of two clusters at low and high redshift using their molecular gas trac
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