On the electron-induced isotope fractionation in low temperature32O2/36O2ices—ozone as a case study

Sivaraman, Bhala; Mebel, Alexander M.; Mason, Nigel J.; Babikov, Dmitri; Kaiser, Ralf I.

doi:10.1039/c0cp00448k

Cited by 12 publications

(7 citation statements)

References 45 publications

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“…This complements and is in agreement with laboratory experiments that find generation of O 2 and O 3 . 2,13,14,17,21,[58][59][60] Such a mechanism for O 2 formation may also be operative at conditions prevalent in the interstellar medium although there, alternative routes such as the reactive O + OH collision are considered to be important, too. 16,17…”

Section: Discussionmentioning

confidence: 99%

O₂ formation in cold environments

Pezzella

Meuwly

2019

Phys. Chem. Chem. Phys.

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Section: Discussionmentioning

confidence: 99%

O₂ formation in cold environments

Pezzella

Meuwly

2019

Phys. Chem. Chem. Phys.

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“…molecular oxygen. Gas phase experiments show a strong isotopic dependence of the formation of ozone (Janssen et al 1999;Mauersberger et al 2003), and recent experiments on ozone synthesis in the solid state induced by electron bombardment yield an even stronger isotopic enrichment (Sivaraman et al 2010) in favor of the heavier isotopolog. The O 2 photodesorption rate will depend directly on the branching ratio between desorption and dissociation, so more detailed studies on this isotope effect are warranted.…”

Section: Oxygen Photodesorptionmentioning

confidence: 99%

Wavelength-dependent UV photodesorption of pure N₂and O₂ices

Fayolle

Bertin

Romanzin

et al. 2013

A&A

125

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Context. Ultraviolet photodesorption of molecules from icy interstellar grains can explain observations of cold gas in regions where thermal desorption is negligible. This non-thermal desorption mechanism should be especially important where UV fluxes are high. Aims. N 2 and O 2 are expected to play key roles in astrochemical reaction networks, both in the solid state and in the gas phase. Measurements of the wavelength-dependent photodesorption rates of these two infrared-inactive molecules provide astronomical and physical-chemical insights into the conditions required for their photodesorption. Methods. Tunable radiation from the DESIRS beamline at the SOLEIL synchrotron in the astrophysically relevant 7 to 13.6 eV range is used to irradiate pure N 2 and O 2 thin ice films. Photodesorption of molecules is monitored through quadrupole mass spectrometry. Absolute rates are calculated by using the well-calibrated CO photodesorption rates. Strategic N 2 and O 2 isotopolog mixtures are used to investigate the importance of dissociation upon irradiation. Results. N 2 photodesorption mainly occurs through excitation of the b 1 Π u state and subsequent desorption of surface molecules. The observed vibronic structure in the N 2 photodesorption spectrum, together with the absence of N 3 formation, supports that the photodesorption mechanism of N 2 is similar to CO, i.e., an indirect DIET (Desorption Induced by Electronic Transition) process without dissociation of the desorbing molecule. In contrast, O 2 photodesorption in the 7−13.6 eV range occurs through dissociation and presents no vibrational structure. Conclusions. Photodesorption rates of N 2 and O 2 integrated over the far-UV field from various star-forming environments are lower than for CO. Rates vary between 10 −3 and 10 −2 photodesorbed molecules per incoming photon.

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“…13,14 Irradiation of such a lm by electrons with energies above $10 eV leads to the dissociation of molecular oxygen to release reactive O atoms which can react with remaining O 2 species. What follows is characteristic of the well-known chemistry in the Earth's stratosphere:…”

Section: O 2 Ice Lmsmentioning

confidence: 99%

Electron induced chemistry: a new frontier in astrochemistry

et al. 2014

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The commissioning of the ALMA array and the next generation of space telescopes heralds the dawn of a new age of Astronomy, in which the role of chemistry in the interstellar medium and in star and planet formation may be quantified. A vital part of these studies will be to determine the molecular complexity in these seemingly hostile regions and explore how molecules are synthesised and survive. The current hypothesis is that many of these species are formed within the ice mantles on interstellar dust grains with irradiation by UV light or cosmic rays stimulating chemical reactions. However, such irradiation releases many secondary electrons which may themselves induce chemistry. In this article we discuss the potential role of such electron induced chemistry and demonstrate, through some simple experiments, the rich molecular synthesis that this may lead to.

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On the electron-induced isotope fractionation in low temperature³²O₂/³⁶O₂ices—ozone as a case study

Cited by 12 publications

References 45 publications

O₂ formation in cold environments

O₂ formation in cold environments

Wavelength-dependent UV photodesorption of pure N₂and O₂ices

Electron induced chemistry: a new frontier in astrochemistry

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On the electron-induced isotope fractionation in low temperature32O2/36O2ices—ozone as a case study

Cited by 12 publications

References 45 publications

O2 formation in cold environments

O2 formation in cold environments

Wavelength-dependent UV photodesorption of pure N2and O2ices

Electron induced chemistry: a new frontier in astrochemistry

Contact Info

Product

Resources

About

On the electron-induced isotope fractionation in low temperature³²O₂/³⁶O₂ices—ozone as a case study

O₂ formation in cold environments

O₂ formation in cold environments

Wavelength-dependent UV photodesorption of pure N₂and O₂ices