On Water Formation in the Interstellar Medium: Laboratory Study of the O+d Reaction on Surfaces

Jing, Dapeng; He, Jiao; Brucato, J. R.; Sio, A. De; Tozzetti, Lorenzo; Vidali, Gianfranco

doi:10.1088/2041-8205/741/1/l9

Cited by 49 publications

(64 citation statements)

References 30 publications

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“…For example, Hiraoka et al (1998) sprayed D atoms over O atoms trapped in an N 2 O matrix at 12 K. The O and D atoms were produced by dissociation of, respectively, N 2 O and D 2 under a dc discharge. Dulieu et al (2010) codeposited O and D atoms produced by dissociating O 2 and D 2 , respectively, onto non-porous amorphous H 2 O ice at 10 K. More recently, Jing et al (2011) deposited D atoms and 18 O (instead of 16 O) at 15-25 K on a synthesized olivine surface. All three groups claimed that D 2 O (HDO) formed during their experiments through surface reactions (1) and (2); however, other O-related species, such as O 2 and O 3 , were also present in or on the samples, and it was difficult to separate information relating to reactions (1) and (2) from the different competing H 2 O-formation channels related to O 2 and O 3 , shown below.…”

Section: H 2 O Formationmentioning

confidence: 99%

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H₂, AT 10 K

Oba

Watanabe

Hama

et al. 2012

ApJ

112

141

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The present study experimentally demonstrated that solid H 2 O is formed through the surface reaction OH + H 2 at 10 K. This is the first experimental evidence of solid H 2 O formation using hydrogen in its molecular form at temperatures as low as 10 K. We further found that H 2 O formation through the reaction OH + H 2 is about one order of magnitude more effective than HDO formation through the reaction OH + D 2 . This significant isotope effect results from differences in the effective mass of each reaction, indicating that the reactions proceed through quantum tunneling.

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Section: H 2 O Formationmentioning

confidence: 99%

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H₂, AT 10 K

Oba

Watanabe

Hama

et al. 2012

ApJ

112

141

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“…These two molecules are thought to be catalyzed by the surface of cold (10−100 K) dust grains composed of silicates or carbonaceous materials. Recently, laboratory experiments have demonstrated that water is easily formed from O atoms (Dulieu et al 2010;Jing et al 2011), but also from O 2 (Oba et al 2009;Ioppolo et al 2010;Chaabouni et al 2012) or even O 3 molecules (Mokrane et al 2009;Romanzin et al 2011) by addition of H atoms. The presence of O, O 2 and O 3 at observable abundances on the surface of grains during ice growth is unlikely because of their high reactivity.…”

Section: Introductionmentioning

confidence: 99%

Production of O₂ through dismutation of H₂O₂ during water ice desorption: a key to understanding comet O₂ abundances

Dulieu

Minissale

Bockelée‐Morvan

2016

A&A

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Context. Detection of molecular oxygen and prediction of its abundance have long been a challenge for astronomers. The low abundances observed in few interstellar sources are well above the predictions of current astrochemical models. During the Rosetta mission, an unexpectedly high abundance of O 2 was discovered in the comet 67P/Churyumov-Gerasimenko's coma. A strong correlation between O 2 and H 2 O productions is observed, whereas no such correlation is observed between O 2 and either of CO or N 2 . Aims. We suggest that the O 2 molecule may be formed during the evaporation of water ice. We propose a possible reaction:, a molecule which should be co-produced during the water ice mantle growth on dust grains. We aim to test this hypothesis under realistic experimental conditions. Methods. We performed two sets of experiments. They consist of producing a mixture of D 2 O and D 2 O 2 via the reaction of O 2 and D on a surface held at 10 K. The first set is made on a silicate substrate, and explores the limit of thin films, in order to prevent any complication due to trapping during the desorption. The second set is performed on a pre-deposited H 2 O ice substrate and mimics the desorption of mixed ice. Results. In thin films, O 2 is produced by the dismutation of H 2 O 2 , even at temperatures as low as 155 K. Mixed with water, H 2 O 2 desorbs after the water ice sublimation and even more desorption of O 2 is observed. Conclusions. H 2 O 2 , synthesised during the growth of interstellar ices (or by later processing), desorbs at the latest stage of the water sublimation and undergoes the dismutation reaction. Therefore an O 2 release in the gas phase should occur at the end of the evaporation of ice mantles. Temperature gradients along the geometry of clouds, or interior of comets, should blend the different stages of the sublimation. Averaged along the whole process, a mean value of the O 2 /H 2 O ratio of a few percent in the gas phase seems plausible.

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“…The provenance of asteroidal water has been questioned and the focus of recent literature (11,12); the apparent consensus as yet suggests a continuum (13)(14)(15) of water accretion between anhydrous asteroids and comets and, based in part from analysis of Stardust cometary grains (16), a possible common origin for their water. Water may affect asteroidal petrology post-accretionally (17) with a conversion of anhydrous to hydrous silicates that is sometimes pervasive, as found represented in petrographic grade 1 (C1) CC; in these samples primary silicate minerals and metals are nearly completely replaced by alteration products (18).…”

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confidence: 99%

Large enantiomeric excesses in primitive meteorites and the diverse effects of water in cosmochemical evolution

Pizzarello

Monroe

Лауретта

2012

Proc. Natl. Acad. Sci. U.S.A.

134

153

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Carbonaceous chondrites are meteoritic fragments of asteroids that avoided the geological reprocessing of larger planets and allow laboratory probing of early solar-nebula materials. Among these, Renazzo-type (CR) chondrites found in Antarctica appear remarkably pristine and are distinguished by abundant organic materials and water-soluble molecules such as amino acids and ammonia. We present a comprehensive analysis of the organic composition of selected CR meteorites of different petrographic classification and compare compounds' abundance and distribution as they may relate to asteroidal aqueous processing and concomitant evolution of the mineral phases. We found that several CR compounds such as amino acids and sugar alcohols are fully represented in stones with no or minimal water exposure indicating a formation that, if solar, preceded parent body processes. The most pristine CRs also revealed natal enantiomeric excesses (ee) of up to 60%, much larger than ever recorded. However, aqueous alteration appears to affect CR soluble organic composition and abundances, in particular some diastereomeric amino acids may gauge its extent by the consequent racemization of their ee.primitive asteroids | abiotic molecular evolution | solar ices | clays C R meteorites are characterized by several petrologic, geochemical, and isotopic features, such as containing large chondrules, high Fe-Ni metal abundances, and distinct wholerock O-isotopic distributions (1). However, only recent comprehensive analyses of the soluble and insoluble organic materials in two pristine* CR2 † meteorites, GRA 95229 (GRA1) and LAP 02342 (LAP) (2, 3) revealed what is possibly their most distinguishing characteristic vis-à-vis other carbonaceous chondrites (CC) types (i.e., soluble organic suites that are overall unique for having a preponderance of water-over solvent-soluble compounds). Ammonia is the most abundant single molecule detected in CR2 water extracts, and amino acids are their largest component, unlike, for example, in the Murchison meteorite where hydrocarbons are the dominant molecular species.Amino acids have been the most captivating findings in CC meteorites since the fall of Murchison (4) because several of the compounds have exact molecular correspondence with biomolecules and possible pre-biotic significance. In intervening studies, however, the detection of a diverse and apparently stochastic suite of compounds in many meteorites made it difficult to propose how this random mix could have found effective chemical pathways toward the origin of life (5). CR2s have significantly changed that perspective with their main compositional abundances of water-soluble and N-containing molecular species.CC materials relied on a long cosmic history for their formation, which spanned solar as well as presolar environments. In particular, the high D and 13 C isotopic enrichments of some CC organic compounds have revealed their lineage from cold cosmic regimes (6). Among CRs, GRA1 amino acids display δD values up to þ7;200‰ (2), the larges...

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On Water Formation in the Interstellar Medium: Laboratory Study of the O+d Reaction on Surfaces

Cited by 49 publications

References 30 publications

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H₂, AT 10 K

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H₂, AT 10 K

Production of O₂ through dismutation of H₂O₂ during water ice desorption: a key to understanding comet O₂ abundances

Large enantiomeric excesses in primitive meteorites and the diverse effects of water in cosmochemical evolution

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On Water Formation in the Interstellar Medium: Laboratory Study of the O+d Reaction on Surfaces

Cited by 49 publications

References 30 publications

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H2, AT 10 K

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H2, AT 10 K

Production of O2 through dismutation of H2O2 during water ice desorption: a key to understanding comet O2 abundances

Large enantiomeric excesses in primitive meteorites and the diverse effects of water in cosmochemical evolution

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Resources

About

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H₂, AT 10 K

WATER FORMATION THROUGH A QUANTUM TUNNELING SURFACE REACTION, OH + H₂, AT 10 K

Production of O₂ through dismutation of H₂O₂ during water ice desorption: a key to understanding comet O₂ abundances