H2 Formation on Grain Surfaces

By S. Cazaux, P. Caselli, M. Walmsley, A. Tielens. Proceedings of the International Astronomical Union, 2004

280 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/39fb35d4c9fd49dcde7a07b7f4296f211a7e8325

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Citations in the corpus

Simulating the Formation of Molecular Clouds. I. Slow Formation by Gravitational Collapse from Static Initial Conditions (2006, background): “This remains widely accepted, at least for cold dust, although there is ongoing debate about the efficacy of H2 formation on warm dust (see e.g. Katz et al. 1999; Cazaux & Tielens 2004).”
Complex organic molecules in protoplanetary disks (2013, methodology): “A reanalysis of this experimental work determined a quantum component is necessary to explain the rate of formation of HD observed in the experiments (Cazaux & Tielens 2004).”
The warm gas atmosphere of the HD 100546 disk seen by Herschel - Evidence of a gas-rich, carbon-poor atmosphere? (2012, methodology): “We then compare the result to our “standard” H2 formation rate using the S × η reported by Cuppen et al. (2010), in order to capture the theoretical work of Cazaux & Tielens (2004), Cuppen & Herbst (2005) as well as the observational evidence from Habart et al. (2004).”
Reaction Networks for Interstellar Chemical Modelling: Improvements and Challenges (2010, methodology): “To use the results from Katz et al. (1999) again as an example, Cazaux and Tielens (2004) and Cuppen and Herbst (2005) were able to fit the same experimental results using different models.”
The big problems in star formation: The star formation rate, stellar clustering, and the initial mass function (2014, methodology): “The quantities H2 and S (T ) can be calculated from models or measured from laboratory experiments (e.g. Hollenbach & McKee 1979; Cazaux & Tielens 2002, 2004; Cazaux et al. 2005), while Σgr can be constrained approximately from the level of dust extinction in the UV (Draine 2003, 2011, and…”
Diagnostics of irradiated gas in galaxy nuclei. I. A far-ultraviolet and X-ray dominated region code (2005, background): “Recently, Cazaux & Tielens (2002, 2004) developed a model for the formation of hydrogen under astrophysically relevant conditions.”
Star Formation at Very Low Metallicity. I. Chemistry and Cooling at Low Densities (2007, background): “However, a recent analysis of H2 formation on grain surfaces by Cazaux & Tielens (2004) that takes both physisorbed (i.e., van der Waals bonded) and chemisorbed (i.e., chemically bonded) hydrogen into account demonstrates that in the conditions of interest in this paper, freact 1 (with the result…”
A Model for Atomic and Molecular Interstellar Gas: The Meudon PDR Code (2006, background): “X; k ¼ ffiffiffiffiffiffiffiffi 2k mX s exp Td ; where is the adsorption binding energy of X on the surface, 2k /mXð Þ1/2 a vibration frequency and Td the dust temperature. see Cazaux & Tielens (2004) for details.”
Survival of molecular gas in cavities of transition disks - I. CO (2013, methodology): “Chemistry The chemical network is taken consistently with Bruderer et al. (2012), except that we use the H2 formation rate by Cazaux & Tielens (2004, 2010).”
A photon dominated region code comparison study (2007, background): “…field, is of major importance for the chemistry in PDRs. H2 forms on grain surfaces, a process which crucially depends on the temperatures of the gas and the grains (Hollenbach & Salpeter 1971; Cazaux & Tielens 2004), which themselves depend on the local cooling and heating, governed by the FUV.”
The Birth of Molecular Clouds: Formation of Atomic Precursors in Colliding Flows (2006, background): “This might appear to be somewhat high, since the sticking probability decreases rapidly with higher temperatures, and is near unity only for T < 20K (Cazaux & Tielens 2004; Bergin et al. 2004).”
Simulating the Formation of Molecular Clouds. II. Rapid Formation from Turbulent Initial Conditions (2006, background): “…physics of H2 formation on dust is believed to be well understood, although uncertainties remain about various issues such as the relative importance of physisorption versus chemisorption (see, e.g., Katz et al. 1999; Cazaux & Tielens 2004) or the role of dust grain porosity (Perets & Biham 2006).”
The formation of molecular clouds in spiral galaxies (2006, background): “For example, the efficiency of grain formation, assumed here to be a constant S = 0.3, can be as high as S = 1 for T < 20 and as low as S ∼ 0.1 for T > 100 K (Cazaux & Tielens 2004).”
Diffuse Atomic and Molecular Clouds (2006, background): “Note that H2 formation may not be as simple as these assumptions suggest (Biham et al. 2001, Cazaux & Tielens 2004).”