Amino acids in meteorites

Cronin, John R.; Pizzarello, Sandra

doi:10.1016/0273-1177(83)90036-4

Cited by 276 publications

(187 citation statements)

References 32 publications

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“…29 4 . We used A = 1.9 Â 10 À16 cm molecule À1 for water, A = 7.1 Â 10 À17 cm molecule À1 for CO 2 , and A = 8.085 Â 10 À18 cm molecule À1 for pure CH 4 ice (corrected assuming a CH 4 density of 0.47 g cm À3 as described by Herrero et al 32 ). To determine glycine column densities we were faced with the problem of lacking experimental information on the integrated absorption coefficient of the glycine bands.…”

Section: Methodsmentioning

confidence: 99%

An infrared study of solid glycine in environments of astrophysical relevance

Maté

Rodrı́guez-Lazcano

Gálvez

et al. 2011

Phys. Chem. Chem. Phys.

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The conversion from neutral to zwitterionic glycine is studied using infrared spectroscopy from the point of view of the interactions of this molecule with polar (water) and non-polar (CO 2 , CH 4 ) surroundings. Such environments could be found on astronomical or astrophysical matter. The samples are prepared by vapour-deposition on a cold substrate (25 K), and then heated up to sublimation temperatures of the co-deposited species. At 25 K, the neutral species is favoured over the zwitterionic form in non-polar environments, whereas for pure glycine, or in glycine/water mixtures, the dominant species is the latter. The conversion is easily followed by the weakening of two infrared bands in the mid-IR region, associated to the neutral structure. Theoretical calculations are performed on crystalline glycine and on molecular glycine, both isolated and surrounded by water. Spectra predicted from these calculations are in reasonable agreement with the experimental spectra, and provide a basis to the assignments. Different spectral features are suggested as probes for the presence of glycine in astrophysical media, depending on its form (neutral or zwitterionic), their temperature and composition.

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Section: Methodsmentioning

confidence: 99%

An infrared study of solid glycine in environments of astrophysical relevance

Maté

Rodrı́guez-Lazcano

Gálvez

et al. 2011

Phys. Chem. Chem. Phys.

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“…A comprehensive knowledge of both solid-state processes and sublimation processes is necessary in order to interpret hot-core observational data and to constrain star formation models. Moreover, we need to know which molecular species will remain on the grain surface after the water ice desorption, to understand which species may participate in a solid-state water-free chemistry, leading to the formation of the complex organic molecules which are detected in meteorites (Cronin & Pizzarello 1983). These refractory molecules constrain the initial abundances of this water-free chemistry that may lead to precursors of biomolecules.…”

Section: Introductionmentioning

confidence: 99%

The desorption of H₂CO from interstellar grains analogues

Noble

Theulé

Mispelaer

et al. 2012

A&A

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Context. Much of the formaldehyde (H 2 CO) is formed from the hydrogenation of CO on interstellar dust grains, and is released in the gas phase in hot core regions. Radio-astronomical observations in these regions are directly related to its desorption from grains. Aims. We study experimentally the thermal desorption of H 2 CO from bare silicate surfaces, from water ice surfaces and from bulk water ice in order to model its desorption from interstellar grains. Methods. Temperature-programmed desorption experiments, monitored by mass spectrometry, and Fourier transform infrared spectroscopy are performed in the laboratory to determine the thermal desorption energies in: (i.) the multilayer regime where H 2 CO is bound to other H 2 CO molecules; (ii.) the submonolayer regime where H 2 CO is bound on top of a water ice surface; (iii.) the mixed submonolayer regime where H 2 CO is bound to a silicate surface; and (iv.) the multilayer regime in water ice, where H 2 CO is embedded within a H 2 O matrix. Results. In the submonolayer regime, we find the zeroth-order desorption kinetic parameters ν 0 = 10 28 mol cm −2 s −1 and E = 31.0 +/− 0.9 kJ mol −1 for desorption from an olivine surface. The zeroth-order desorption kinetic parameters are ν 0 = 10 28 mol cm −2 s −1 and E = 27.1 +/− 0.5 kJ mol −1 for desorption from a water ice surface in the submonolayer regime. In a H 2 CO:H 2 O mixture, the desorption is in competition with the H 2 CO + H 2 O reaction, which produces polyoxymethylene, the polymer of H 2 CO. This polymerization reaction prevents the volcano desorption and co-desorption from happening. Conclusions. H 2 CO is only desorbed from interstellar ices via a dominant sub-monolayer desorption process (E = 27.1 +/− 0.5 kJ mol −1 ). The H 2 CO which has not desorbed during this sub-monolayer desorption polymerises upon reaction with H 2 O, and does not desorb as H 2 CO at higher temperature.

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“…For example, 52 amino acids have been identified in the Murchison meteorite. Thirty three of these amino acids are unknown in natural materials [11]. However, as reported above, amino acids were also found in the acidic hydrolysis of tholins coming from N 2 -CH 4 mixtures subjected to electric shocks, a gaseous composition free of any oxygenated compounds.…”

Section: Amino Acids In Meteoritesmentioning

confidence: 68%

Amino Acids in the Universe

Guillemin

2014

BIO Web of Conferences

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Abstract.What is the role played by amino acids in the chemistry of the interstellar medium and the emergence of life on the early Earth? Are they really the primary key compounds as free amino acids? Is their presence or absence in the interstellar medium a significant problem? How to get an amino acid sample with an enantiomeric excess on the early Earth or ISM? How to increase the enantiomeric excess to have pure enantiomers? All these questions have received partial answers but they remain open and probably they will still be open for several more decades.

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Amino acids in meteorites

Cited by 276 publications

References 32 publications

An infrared study of solid glycine in environments of astrophysical relevance

An infrared study of solid glycine in environments of astrophysical relevance

The desorption of H₂CO from interstellar grains analogues

Amino Acids in the Universe

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Amino acids in meteorites

Cited by 276 publications

References 32 publications

An infrared study of solid glycine in environments of astrophysical relevance

An infrared study of solid glycine in environments of astrophysical relevance

The desorption of H2CO from interstellar grains analogues

Amino Acids in the Universe

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The desorption of H₂CO from interstellar grains analogues