Detection of cometary amines in samples returned by Stardust

Glavin, Daniel P.; Dworkin, Jason P.; Sandford, Scott A.

doi:10.1111/j.1945-5100.2008.tb00629.x

Cited by 122 publications

(113 citation statements)

References 55 publications

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“…Its presence in interstellar ices is strengthened by its detection in volatile compounds coming from cometary surface (Glavin et al 2008). Consequently, by taking into account the above arguments and the results obtained in this work, we suggest that acetonitrile can be synthesized at the surface of interstellar or cometary grains following a two step dehydrogenation of ethylamine under VUV irradiation.…”

Section: Astrophysical Discussionmentioning

confidence: 94%

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Experimental investigation of nitrile formation from VUV photochemistry of interstellar ices analogs: acetonitrile and amino acetonitrile

Danger

Bossa

Marcellus

et al. 2010

A&A

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Context. The study of the chemical reactivity in interstellar ices in astrophysical environments is an important tool for understanding the origin of the organic matter in molecular clouds, in protoplanetary disks, and possibly, as a final destination, in our solar system. The laboratory simulations of the reactivity in ice analogs provide important information for understanding the reactivity in these environments. Here, we used these experimental simulations to trace some formation pathways of two nitriles, acetonitrile and amino acetonitrile, which are two potential precursors of amino acids in astrophysical environments. Aims. The purpose of this work is to present the first experimental approach for the formation of acetonitrile and amino acetonitrile in interstellar-like conditions. Methods. We use Fourier Transform InfraRed (FTIR) spectroscopy and mass spectrometry to study the formation at 20 K of acetonitrile CH 3 CN from VUV irradiation of ethylamine and of amino acetonitrile NH 2 CH 2 CN from VUV irradiation of ammonia: acetonitrile mixture. Isotopic substitutions are used to confirm identifications. Results. We demonstrate that acetonitrile can be formed at 20 K from the VUV irradiation of ethylamine with a yield of 4%. Furthermore, in presence of ammonia, at 20 K and under VUV irradiation, the acetonitrile can lead to the amino acetonitrile formation. These results suggest that acetonitrile and amino acetonitrile can be formed in astrophysical environments that are submitted to VUV irradiations.

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Section: Astrophysical Discussionmentioning

confidence: 94%

“…In particular, ethylamine has been identified in the cometexposed materials from stardust (Glavin et al 2008). Different pathways for ethylamine formation were already suggested for these environments.…”

Section: Astrophysical Discussionmentioning

confidence: 99%

Experimental investigation of nitrile formation from VUV photochemistry of interstellar ices analogs: acetonitrile and amino acetonitrile

Danger

Bossa

Marcellus

et al. 2010

A&A

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“…In cometary coma, approximately 25 molecules have been detected by radio astronomy (Crovisier et al 1998;Bockelée-Morvan et al 2000;Despois 1999;Irvine et al 2000), but not glycine (Ehrenfreund et al 2002;Crovisier et al 2004). Finally, within the returned samples of comet 81P/Wild 2 from the Stardust mission, traces of glycine and β-alanine have been detected as well as amines such as methylamine and ethylamine (Sandford et al 2006;Glavin 2008). An open question is whether glycine can be synthesized in these environments.…”

Section: Introductionmentioning

confidence: 99%

Methylammonium methylcarbamate thermal formation in interstellar ice analogs: a glycine salt precursor in protostellar environments

Bossa¹,

Duvernay²,

Theulé³

et al. 2009

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Context. Analyses of dust cometary grains collected by the Stardust spacecraft have shown the presence of amines and amino acids molecules, and among them glycine (NH 2 CH 2 COOH). We show how the glycine molecule could be produced in the protostellar environments before its introduction into comets. Aims. We study the evolution of the interstellar ice analogues affected by both thermal heating and vacuum ultraviolet (VUV) photons, in addition to the nature of the formed molecules and the confrontation of our experimental results with astronomical observations. Methods. Infrared spectroscopy and mass spectrometry are used to monitor the evolution of the H 2 O:CO 2 :CH 3 NH 2 and CO 2 :CH 3 NH 2 ice mixtures during both warming processes and VUV photolysis. Results. We first show how carbon dioxide (CO 2 ) and methylamine (CH 3 NH 2 ) thermally react in water-dominated ice to form methylammonium methylcarbamate [CH 3 NH + 3 ][CH 3 NHCOO − ] noted C. We then determine the reaction rate and activation energy. We show that C thermal formation can occurs in the 50-70 K temperature range of a protostellar environment. Secondly, we report that a VUV photolysis of a pure C sample produces a glycine salt, methylammonium glycinate [CH 3 NH + 3 ][NH 2 CH 2 COO − ] noted G. We propose a scenario explaining how C and subsequently G can be synthesized in interstellar ices and precometary grains. Conclusions. [CH 3 NH + 3 ][CH 3 NHCOO − ] could be readily formed and would act as a glycine salt precursor in protostellar environments dominated by thermal and UV processing. We propose a new pathway leading to a glycine salt, which is consistent with the detection of glycine and methylamine within the returned samples of comet 81P/Wild 2 from the Stardust mission.

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“…Precise analyses of single comet particles can strongly constrain the chemistry and timescale of solar system formation. The discovery of cometary amines in Stardust material [Glavin et al, 2008] supports the hypothesis that comets were an important source of prebiotic organic carbon and nitrogen on the early Earth.…”

Section: Comet Particles From the Stardust Spacecraftmentioning

confidence: 48%