Photoionization mass spectrometry of NH2OH: Heats of formation of HNO+ and NOH+

Kutina, R. E.; Goodman, G. L.; Berkowitz, J.

doi:10.1063/1.444062

Cited by 29 publications

(14 citation statements)

References 26 publications

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“…The repetition of several cycles enhances the signal-to-noise ratio of the QMS ion count upon ice sublimation. In the figure, signals are recorded at m/z = 33 (NH 2 OH) as well as 30 (NO), 17 (OH), and 16 (NH 2 ), reflecting partial fragmentation upon NH 2 OH ionization in the QMS head (Kutina et al 1982). All signals have a common peak at T ∼ 188 K, confirming NH 2 OH fragmentation upon ionization.…”

Section: Resultsmentioning

confidence: 89%

NO ICE HYDROGENATION: A SOLID PATHWAY TO NH ₂ OH FORMATION IN SPACE

Congiu

Fedoseev

Ioppolo

et al. 2012

ApJ

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Icy dust grains in space act as catalytic surfaces onto which complex molecules form. These molecules are synthesized through exothermic reactions from precursor radicals and, mostly, hydrogen atom additions. Among the resulting products are species of biological relevance, such as hydroxylamine-NH 2 OH-a precursor molecule in the formation of amino acids. In this Letter, laboratory experiments are described that demonstrate NH 2 OH formation in interstellar ice analogs for astronomically relevant temperatures via successive hydrogenation reactions of solid nitric oxide (NO). Inclusion of the experimental results in an astrochemical gas-grain model proves the importance of a solid-state NO + H reaction channel as a starting point for prebiotic species in dark interstellar clouds and adds a new perspective to the way molecules of biological importance may form in space.

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Section: Resultsmentioning

confidence: 89%

NO ICE HYDROGENATION: A SOLID PATHWAY TO NH ₂ OH FORMATION IN SPACE

Congiu

Fedoseev

Ioppolo

et al. 2012

ApJ

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“…The signals are recorded at m/z = 33 (NH 2 OH) as well as 30 (NO), 17 (OH), and 16 (NH 2 ), reflecting partial fragmentation upon NH 2 OH ionization in the QMS head. 42 Fig. 4(c) result from the NO + D experiment performed on crystalline water ice and appear to have a different behavior from the two preceding cases.…”

Section: B Formation Of Hydroxylaminementioning

confidence: 80%

Efficient surface formation route of interstellar hydroxylamine through NO hydrogenation. I. The submonolayer regime on interstellar relevant substrates

Congiu

Chaabouni

Laffon

et al. 2012

The Journal of Chemical Physics

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Dust grains in the interstellar medium are known to serve as the first chemical laboratory where the rich inventory of interstellar molecules are synthesized. Here we present a study of the formation of hydroxylamine--NH(2)OH--via the non-energetic route NO + H (D) on crystalline H(2)O and amorphous silicate under conditions relevant to interstellar dense clouds. Formation of nitrous oxide (N(2)O) and water (H(2)O, D(2)O) is also observed and the reaction network is discussed. Hydroxylamine and water results are detected in temperature-programmed desorption (TPD) experiments, while N(2)O is detected by both reflection-absorption IR spectroscopy and TPD techniques. The solid state NO + H reaction channel proves to be a very efficient pathway to NH(2)OH formation in space and may be a potential starting point for prebiotic species in dark interstellar clouds. The present findings are an important step forward in understanding the inclusion of interstellar nitrogen into a non-volatile aminated species since NH(2)OH provides a solid state nitrogen reservoir along the whole evolutionary process of interstellar ices from dark clouds to planetary systems.

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“…9) which have singlet ground states. 41 The observation that metastables affect the NO + /H20 + branching ratios in the SIFt' studies is, therefore, not surprising. Spin-conservation rules prohibit ground-state reactants to access the ground states of the intermediates.…”

Section: Ha'a(ro) Is the Pure Electronic Coupling (V'!v') Is Thementioning

confidence: 95%