Carbonaceous components in the comet Halley dust

Fomenkova, M. N.; Chang, Sherwood; Mukhin, L. M.

doi:10.1016/0016-7037(94)90351-4

Cited by 98 publications

(54 citation statements)

References 57 publications

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“…A large fraction of the cometary organics, about 50%, are oxygen-rich (O/C ≥ 0.4); these compounds are consistent with structures of alcohols, aldehydes, ketones, acids and amino acids, and their salts, although the exact makeup of these molecules can not be unambiguously identified (Fomenkova 1994(Fomenkova , 1999. The O/C ratio of the oxygen-rich fraction in comets is similar to the residue of the standard experiment, OR1 (Sect.…”

Section: Astrophysical Implicationssupporting

confidence: 54%

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UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results

Muñoz

Schütte

2003

A&A

162

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Abstract. We simulate experimentally the physical conditions present in dense clouds by means of a high vacuum experimental setup at low temperature T ≈ 12 K. The accretion and photoprocessing of ices on grain surfaces is simulated in the following way: an ice layer with composition analogous to that of interstellar ices is deposited on a substrate window, while being irradiated by ultraviolet (UV) photons. Subsequently the sample is slowly warmed up to room temperature; a residue remains containing the most refractory products of photo-and thermal processing. In this paper we report on the Fourier transform-infrared (FT-IR) spectroscopy of the refractory organic material formed under a wide variety of initial conditions (ice composition, UV spectrum, UV dose and sample temperature). The refractory products obtained in these experiments are identified and the corresponding efficiencies of formation are given. The first evidence for carboxylic acid salts as part of the refractory products is shown. The features in the IR spectrum of the refractory material are attributed to hexamethylenetetramine (HMT, [(CH 2 ) 6 N 4 ]), ammonium salts of carboxylic acids [(R-COO − )(NH + )], amides [H 2 NC(=O)-R], esters [R-C(=O)-O-R ] and species related to polyoxymethylene (POM, [(-CH 2 O-) n ]). Furthermore, evidence is presented for the formation of HMT at room temperature, and the important role of H 2 O ice as a catalyst for the formation of complex organic molecules. These species might also be present in the interstellar medium (ISM) and form part of comets. Ongoing and future cometary missions, such as Stardust and Rosetta, will allow a comparison with the laboratory results, providing new insight into the physico-chemical conditions present during the formation of our solar system.

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Section: Astrophysical Implicationssupporting

confidence: 54%

“…The large abundances of oxygen-rich complex organic molecules found in comet Halley (Kissel & Krueger 1987;Fomenkova et al 1994) suggests that energetic processing in the ISM, and/or the solar nebula, cannot be disregarded.…”

Section: Photoprocessing Of Ices In the Ismmentioning

confidence: 99%

UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results

Muñoz

Schütte

2003

A&A

162

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“…They are also rich in organic molécules. Indeed, organic molecules have been detected in cometary grains by in-situ mass spectrometry (Kissel & Krueger 1987;Fomenkova et al 1994;Kissel et al 2004). The delivery of these organic species to the surface of the early Earth by comets may have provided the basic ingredients required for the origin of life (Oró 1961;Bernstein et al 2002;Muñoz Caro et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Importance of thermal reactivity for hexamethylenetetramine formation from simulated interstellar ices

Vinogradoff

Fray

Duvernay

et al. 2013

A&A

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Context. Complex organic molecules are observed in a broad variety of astrophysical objects, but little is known about their formation mechanism. Laboratory simulations on interstellar ice analogues are therefore crucial for understanding the origin of these complex organic molecules. In this context, we focus on the thermal reactivity for the formation of the organic residue obtained after photolysis at 25 K of the interstellar ice analogue (H 2 O:CH 3 OH:NH 3 ) warmed to 300 K. Aims. We determine the formation mechanism of one major product detected in the organic residue: hexamethylenetetramine (HMT). We compare the warming of the photolysed interstellar ice analogue with the warming of the two non-photolysed specific ice mixtures H 2 CO:NH 3 :HCOOH and CH 2 NH:HCOOH, which are used as references. Using both general and specific approaches, we show the precise role of the UV photons and the thermal processing in the HMT formation. Methods. We used Fourier transform infrared spectroscopy (FTIR) to monitor the chemical changes induced by the heating of the photolysed ice analogue and characterize some important species that will subsequently evolve in the formation of HMT in the residue. Results. We show that the thermal processes play a key role in the HMT formation in photolysed ice analogues heated at 300 K. We identify the stable intermediates in the HMT formation that are formed during the warming: the aminomethanol (NH 2 CH 2 OH) and the protonated ion trimethyletriamine (TMTH + , C 3 H 10 N + 3 ). We also identify for the first time a new product in the organic residue, the polymethylenimine PMI (-(CH 2 -NH) n ). Results from this study will be interesting for the analysis of the forthcoming Rosetta mission.

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“…11b), corresponding to N concentrations between 1 -6 wt.%, which is at the upper end of the range of N concentrations of insoluble organic matter in carbonaceous chondrites (Aléon et al, 2003). A wide variety of CHON grains (composed predominantly of the elements C, H, O, and N) detected in dust from the comet Halley (Jessberger et al, 1988) have N concentrations in this range, and it has been suggested that these may represent organic compounds such as alcohols, ketones, aldehydes, amines and amino acids, with the presence of N indicating amine or nitrile functionalities (Fomenkova et al, 1994). Several hotspots have higher CN -/C -ratios of 2 -3.5, suggesting N concentrations of 10 -30 wt.%.…”

Section: Nitrogen Isotopic Distributions and Carriers In Idpsmentioning

confidence: 99%

Identification of isotopically primitive interplanetary dust particles: A NanoSIMS isotopic imaging study

Floss

Stadermann

Bradley

et al. 2006

Geochimica et Cosmochimica Acta

199

285

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We have carried out a comprehensive survey of the isotopic compositions (H, B, C, N, O, S) of a suite of interplanetary dust particles (IDPs), including both cluster and individual particles. Isotopic imaging with the NanoSIMS shows the presence of numerous discrete hotspots that are strongly enriched in 15 Based on their N isotopic compositions, the IDPs studied here can be divided into two groups. One group is characterized as being "isotopically primitive" and consists of those IDPs that have anomalous bulk N isotopic compositions. These particles typically also contain numerous 15 N-rich hotspots, occasional C isotopic anomalies, and abundant presolar silicate grains. In contrast, the other "isotopically normal" IDPs have normal bulk N isotopic compositions and, although some contain 15 N-rich hotspots, none exhibit C isotopic anomalies and none contain presolar silicate or oxide grains. Thus, isotopically interesting IDPs can be identified and selected on the basis of their N isotopic compositions for further study. However, isotopes. This may be due to different effects of secondary processing on the isotopic systems involved.3

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Carbonaceous components in the comet Halley dust

Cited by 98 publications

References 57 publications

UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results

UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results

Importance of thermal reactivity for hexamethylenetetramine formation from simulated interstellar ices

Identification of isotopically primitive interplanetary dust particles: A NanoSIMS isotopic imaging study

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