Relevant bibliographies by topics / Hydrogène interstellaire – Composition

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  1. Journal articles
  2. Dissertations / Theses
  3. Book chapters

Academic literature on the topic 'Hydrogène interstellaire – Composition'

Author: Grafiati
Published: 4 June 2021
Last updated: 14 February 2022

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Journal articles on the topic "Hydrogène interstellaire – Composition"

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Gredel, R., S. Lepp, A. Dalgarno, and E. Herbst. "Cosmic Ray Induced Photodestruction of Interstellar Molecules." International Astronomical Union Colloquium 120 (1989): 32–37. http://dx.doi.org/10.1017/s0252921100023459.

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AbstractUltraviolet photons are created in the interior of dense interstellar clouds by the impact excitation of molecular hydrogen by secondary electrons generated by cosmic ray ionization. The resulting photodissociation and photoionization rates of a wide range of interstellar molecules are calculated. The effects on the equilibrium chemical composition of dense clouds are briefly discussed.
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Krankowsky, Dieter. "The Composition of Comets." International Astronomical Union Colloquium 116, no. 2 (1991): 854–77. http://dx.doi.org/10.1017/s0252921100012744.

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Abstract.The chemical composition of gases in the coma of Comet Halley obtained from in situ and remote observations is reviewed. Water vapor with an abundance of approximately 80% by number is the dominant parent gas. Carbon monoxide is the second most abundant molecule, with about one-seventh of the water abundance. The other expected parent gases—carbon dioxide, methane, and ammonia—contributed with at most a few percent to the coma gas. Molecular nitrogen is found to be a minor species, with an abundance of less than one percent. Formaldehyde is relatively abundant, with a few percent rela
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Steinwandel, Ulrich P., Benjamin P. Moster, Thorsten Naab, Chia-Yu Hu, and Stefanie Walch. "Hot phase generation by supernovae in ISM simulations: resolution, chemistry, and thermal conduction." Monthly Notices of the Royal Astronomical Society 495, no. 1 (2020): 1035–60. http://dx.doi.org/10.1093/mnras/staa821.

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ABSTRACT Supernovae (SNe) generate hot gas in the interstellar medium (ISM), help setting the ISM structure, and support the driving of outflows. It is important to resolve the hot gas generation for galaxy formation simulations at solar mass and sub-parsec resolution that realize individual SN explosions with ambient densities varying by several orders of magnitude in a realistic multiphase ISM. We test resolution requirements by simulating SN blast waves at three metallicities (Z = 0.01, 0.1, and 1 Z⊙), six densities and their respective equilibrium chemical compositions (n = 0.001–100 cm−3)
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Simons, M. A. J., T. Lamberts, and H. M. Cuppen. "Formation of COMs through CO hydrogenation on interstellar grains." Astronomy & Astrophysics 634 (February 2020): A52. http://dx.doi.org/10.1051/0004-6361/201936522.

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Context. Glycoaldehyde, ethylene glycol, and methyl formate are complex organic molecules that have been observed in dark molecular clouds. Because there is no efficient gas-phase route to produce these species, it is expected that a low-temperature surface route existst that does not require energetic processing. CO hydrogenation experiments at low temperatures showed that this is indeed the case. Glyoxal can form through recombination of two HCO radicals and is then further hydrogenated. Aims. Here we aim to constrain the methyl formate, glycolaldehyde, and ethylene glycol formation on the s
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Williams, David A. "Grains in Diffuse Clouds: Carbon-Coated Silicate Cores." Symposium - International Astronomical Union 135 (1989): 367–73. http://dx.doi.org/10.1017/s0074180900125379.

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A new model of interstellar grains is proposed in which grains in diffuse clouds consist of small (radius ≲ 10nm) and large asymmetric (0.05μm – 0.25μm) silicate cores thinly coated with mantles of amorphous carbon (thickness ≲ 5nm). This model can account successfully for many of the observed properties of interstellar dust and gives a simple interpretation of the interstellar extinction curve. The extinction bump at 220nm is attributed to absorption by finely divided silicates, as indicated by laboratory data. The large silicates provide a “grey” background extinction through the visual and
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Echiburú, C. S., S. Guillot, Y. Zhao, C. O. Heinke, F. Özel, and N. A. Webb. "Spectral analysis of the quiescent low-mass X-ray binary in the globular cluster M30." Monthly Notices of the Royal Astronomical Society 495, no. 4 (2020): 4508–17. http://dx.doi.org/10.1093/mnras/staa1456.

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ABSTRACT We present a recent Chandra observation of the quiescent low-mass X-ray binary containing a neutron star (NS), located in the globular cluster M30. We fit the thermal emission from the NS to extract its mass and radius. We find no evidence of flux variability between the two observations taken in 2001 and 2017, nor between individual 2017 observations, so we analyse them together to increase the signal-to-noise ratio. We perform simultaneous spectral fits using standard light-element composition atmosphere models (hydrogen or helium), including absorption by the interstellar medium, c
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Szécsi, Dorottya, Jonathan Mackey, and Norbert Langer. "Supergiants and their shells in young globular clusters." Astronomy & Astrophysics 612 (April 2018): A55. http://dx.doi.org/10.1051/0004-6361/201731500.

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Context. Anomalous surface abundances are observed in a fraction of the low-mass stars of Galactic globular clusters, that may originate from hot-hydrogen-burning products ejected by a previous generation of massive stars. Aims. We aim to present and investigate a scenario in which the second generation of polluted low-mass stars can form in shells around cool supergiant stars within a young globular cluster. Methods. Simulations of low-metallicity massive stars (Mi ~ 150−600 M⊙) show that both core-hydrogen-burning cool supergiants and hot ionizing stellar sources are expected to be present s
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Stringfellow, Guy S., and Stuart Bowyer. "Modelling the Soft X-Ray and EUV Emission in Classical Novae: EUVE and ROSAT Observations of V1974 Cygni." International Astronomical Union Colloquium 152 (1996): 401–5. http://dx.doi.org/10.1017/s0252921100036290.

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We have conducted an extensive analysis of the observability of Classical Novae with the EUVE Lex/B and Al/Ti/C detectors. Predicted count rates have been computed using optically thin, isothermal plasma models for solar and metal-rich compositions, and hot ONeMg white dwarf model atmospheres. We find EUVE to be quite sensitive to both the EUV and soft X-ray emission emitted by the underlying hot white dwarf during novae outbursts, except for the coolest temperatures with very high intervening hydrogen column density. These results are used to interpret the emission detected during the EUVE al
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Kamiński, Tomek, Karl M. Menten, Romuald Tylenda, et al. "Molecular remnant of Nova 1670 (CK Vulpeculae)." Astronomy & Astrophysics 644 (December 2020): A59. http://dx.doi.org/10.1051/0004-6361/202038648.

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CK Vul erupted in 1670 and is considered a Galactic stellar-merger candidate. Its remnant, observed 350 yr after the eruption, contains a molecular component of surprisingly rich composition, including polyatomic molecules as complex as methylamine (CH3NH2). We present interferometric line surveys with subarcsec resolution with ALMA and SMA. The observations provide interferometric maps of molecular line emission at frequencies between 88 and 243 GHz that allow imaging spectroscopy of more than 180 transitions of 26 species. We present, classify, and analyze the different morphologies of the e
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Christianson, Drew A., and Robin T. Garrod. "Chemical Kinetics Simulations of Ice Chemistry on Porous Versus Non-Porous Dust Grains." Frontiers in Astronomy and Space Sciences 8 (April 15, 2021). http://dx.doi.org/10.3389/fspas.2021.643297.

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The degree of porosity in interstellar dust-grain material is poorly defined, although recent work has suggested that the grains could be highly porous. Aside from influencing the optical properties of the dust, porosity has the potential to affect the chemistry occurring on dust-grain surfaces, via increased surface area, enhanced local binding energies, and the possibility of trapping of molecules within the pores as ice mantles build up on the grains. Through computational kinetics simulations, we investigate how interstellar grain-surface chemistry and ice composition are affected by the p
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Dissertations / Theses on the topic "Hydrogène interstellaire – Composition"

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Barriault, Léo. "Étude de la transition entre le gaz atomique et le gaz moléculaire dans deux cirrus de la boucle céleste nord." Thesis, Université Laval, 2010. http://www.theses.ulaval.ca/2010/27486/27486.pdf.

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Book chapters on the topic "Hydrogène interstellaire – Composition"

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Binney, James. "2. Gas between the stars." In Astrophysics: A Very Short Introduction. Oxford University Press, 2016. http://dx.doi.org/10.1093/actrade/9780198752851.003.0002.

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The space between stars is taken up by gas—mostly hydrogen and helium—which manifests itself in many ways, the most important being the absorption of starlight. ‘Gas between the stars’ describes interstellar absorption and the reddening of stars—when dust grains in the gas absorb blue and ultraviolet light, but let red light from the Sun pass through. These dust grains play a crucial role in regulating the temperature, density, and chemical composition of the gas. This composition of interstellar gas hinges on the balance between the destructive power of ultraviolet photons and the catalytic action of dust grains.
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