OH Molecules in the Interstellar Medium

Robinson, B. J.; McGee, R. X.

doi:10.1146/annurev.aa.05.090167.001151

Cited by 67 publications

(30 citation statements)

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“…[1][2][3][4][5][6] In addition, both ethanol and OH have been detected in interstellar molecular clouds and star forming regions (hot and cold cores) such as W3(OH) and Sgr B2, where temperatures can reach as low as 40 K. [7][8][9][10][11][12][13] Millar et al 12 suggested that ethanol could potentially be used as a chemical clock for hot cores if the kinetics of its reactions with species including the hydroxyl radical were better understood at temperatures pertinent to such environments. Conducting kinetic studies with species known to be present in these cold environments is important for the advancement of chemical models of these regions.…”

Section: Introductionmentioning

confidence: 99%

Measurements of Rate Coefficients for Reactions of OH with Ethanol and Propan-2-ol at Very Low Temperatures

et al. 2014

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The low temperature kinetics of the reactions of OH with ethanol and propan-2-ol have been studied using a pulsed Laval nozzle apparatus coupled with pulsed laser photolysis -laser induced fluorescence (PLP-LIF) spectroscopy. The rate coefficients for both reactions have been found to increase significantly as the temperature is lowered, by~a factor of 18 between 293 and 54 K for ethanol, and by~10 between 298 and 88 K for OH + propan-2-ol. The pressure dependence of the rate coefficients provide evidence for two reaction channels; a zero pressure bimolecular abstraction channel leading to products and collisional stabilization of a weakly bound OH-alcohol complex. The presence of the abstraction channel at low temperatures is rationalized by a quantum mechanical tunneling mechanism, most likely through the barrier to hydrogen abstraction from the OH moiety on the alcohol.

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Section: Introductionmentioning

confidence: 99%

Measurements of Rate Coefficients for Reactions of OH with Ethanol and Propan-2-ol at Very Low Temperatures

et al. 2014

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“…Indeed, many studies have proved that the OH radical, even present at low concentration in the troposphere, reacts efficiently with many trace species, including poisonous carbon monoxide, the greenhouse gas methane, sulphur dioxide and the nitrogen oxides, and other hazardous compounds (Comes 1994; Sennikov, Ignatov & Schrems 2005). OH radicals have been experimentally observed in interstellar space (Robinson & McGee 1967; Baud & Wouterloot 1980; Storey, Watson & Townes 1981). These radicals can be generated by the photodissociation of water (Bergeron et al 2008; Watanabe & Kouchi 2008).…”

Section: Introductionmentioning

confidence: 99%

Production and isolation of OH radicals in water ice

Zins

Joshi

Krim

2011

Monthly Notices of the Royal Astronomical Society

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OH radicals may play an important role in reactions that take place on interstellar icy grain surfaces, due to their high reactivity. Unfortunately, laboratory experiments aiming at simulating such reactions are hindered by the high reactivity of these species. Indeed, a method to isolate and further study the reactivity of OH radicals is still missing. This paper presents a study we carried out to determine the best conditions to isolate OH radicals in water ice. OH radicals were produced using a microwave discharge from either pure gaseous water or a gaseous mixture containing diluted water. Species thus formed were further condensed on a cold mirror at temperatures ranging from 3.5 to 30 K. The samples were then probed with a Fourier transform infrared spectrometer. The dilution of water into a rare gas (He, Ne) was found to be the best way to form an ice containing a high proportion of OH radicals, especially at low temperatures. These conditions, namely low temperatures and low concentrations, allow for the cooling of species formed during the discharge and prevent radical recombination.

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“…Within this perspective we propose an entirely new exothermic reaction path for the formation of serine through some A&A 563, A55 (2014) detected interstellar molecules and radicals, viz., CH (Naylor et al 2010;Gerin et al 2010), CO (Latter et al 1993), NH 2 (Dishoecck 1993;Kerns et al 1972), CH 2 (Polehampton 2005;Hollis et al 1995), and the hydroxyl group OH, an oxygenrich source in the ISM, (Robinson et al 1967;Storey et al 1981;Weinreb et al 1963;Barrett 1964;Ziurys 2006). These molecules and radicals are abundant in the ISM.…”

Section: Introductionmentioning

confidence: 99%

Quantum-chemical approach to serine formation in the interstellar medium: A possible reaction pathway

Singh

Gupta

Misra

et al. 2014

A&A

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Radical-radical and radical-neutral interaction schemes are very important for the formation of comparatively complex molecules in low-temperature chemistry. The formation of amino acids, such as serine, in the interstellar medium is quite difficult. We explored the possibility of serine formation in the interstellar medium through detected interstellar molecules such as CH, CO, and OH by radicalradical and radical-neutral interactions in the gaseous phase using rigorous quantum-chemical calculations. The reaction energies, the low potential barrier and the structures of all the geometries involved in the reaction path show that serine formation is possible in interstellar space via the reaction paths.

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OH Molecules in the Interstellar Medium

Cited by 67 publications

References 0 publications

Measurements of Rate Coefficients for Reactions of OH with Ethanol and Propan-2-ol at Very Low Temperatures

Measurements of Rate Coefficients for Reactions of OH with Ethanol and Propan-2-ol at Very Low Temperatures

Production and isolation of OH radicals in water ice

Quantum-chemical approach to serine formation in the interstellar medium: A possible reaction pathway

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