JpGU-AGU Joint Meeting 2017

Presentation information

[JJ] Poster

P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS09] [JJ] Origin and evolution of materials in space

Mon. May 22, 2017 10:45 AM - 12:15 PM Poster Hall (International Exhibition Hall HALL7)

convener:Shogo Tachibana(Department of Natural History Scieces, Hokkaido University), Hitoshi Miura(Graduate School of Natural Sciences, Department of Information and Basic Science, Nagoya City University), Takafumi Ootsubo(Graduate School of Arts and Sciences, University of Tokyo), Hideko Nomura(Department of Earth and Planetary Sciences, Tokyo Institute of Technology)

[PPS09-P03] N-heterocyclic compound synthesis from aldehydes and ketone with ammonia: A simulation of organic reactions on the meteorite parent bodies

*Junya Miyazaki1, Hiroshi Naraoka1, Akira Tsuchiyama2 (1.Department of Earth and Planetary Sciences Kyushu University, 2.Division of Earth and Planetary Sciences Kyoto University)

Keywords:Chemical Evolution, Mineral-organic interaction, Aqueous alterlation, N-Containing Compound, Carbonaceous chondrite

Carbonaceous chondrites have the most primitive chemical compositions in the solar system and contain volatile components such as water and carbon. In spite of their primitive character, most carbonaceous chondrites have had experienced aqueous alteration on parent bodies, which was revealed by the occurrence of hydrous minerals. The meteoritic carbon are present mainly as organic matter, in which soluble organic matter (SOM, ~1 to ~30 wt%) consists of relatively low-molecular-weight compounds such as carboxylic acids and amino acids. The rest major carbon exists as insoluble organic matter (IOM) having high-molecular complicated structures. Therefore, the aqueous alteration must have influenced the organic-mineral interactions. In order to study the chemical evolution of organic matter in the solar system, the role(s) of minerals should be clarified. In this study, we performed simulation experiments of organic compound synthesis using ammonia (NH3), formaldehyde (HCHO), acetaldehyde (CH3CHO), propionaldehyde (C2H5CHO) and acetone (CH3COCH3), which are simple molecules found in molecular clouds, under the aqueous environment in the presence or absence of minerals.
[Materials and Methods]
The several aqueous mixtures with various ratios (by mol) of NH3 (1 to 10) /HCHO (0.1 to 1) /CH3CHO (0.01 to 0.1) /C2H5CHO (0.01 to 0.1)/CH3COCH3(0.01 to 0.1) were heated in the presence of powdered mineral including forsterite (San Carlos), magnetite (Utah), synthetic forsterite or amorphous silicate (Mg2SiO4 in composition) at 60 to 80℃ for 144 to 192 hours in N2-purged glass ampoules. A total of 20 runs of simulation experiments were performed. The reaction product was extracted with methylene chloride/methanol (2/1, by volume) and analyzed by high performance liquid chromatography/mass spectrometery.
[Results and Discussion]
Many compounds were observed at the range of m/z 100-400 in all reaction products. Of the identified compounds, alkylpyridines (CnH2n-5N), alkylimidazoles (CnH2n-3N2) and hexamethylenetetramine (C6H12N4, HMT) were the main products for each run. The compounds that have not been identified but represented by compositional having CnH2n-1N3O in composition were also identified as a main product. Although alkylpyridines and alkylimidazoles have been detected from carbonaceous chondrites (e.g. Yamashita and Naraoka, 2014). Although HMT has been reported as a main product during interstellar analog experiment by UV irradiation at low temperature (Vinogradoff et al., 2011), HMT has not been found in meteorites. HMT is relatively abundant in the products with the absence of minerals. However, the HMT amount decreased in the presence of the amorphous silicate and forsterite (San Carlos), instead of increasing production of alkylpyridines and alkylimidazoles. The minerals could control the reaction pathways as a catalyst. In particular, as amorphous silicate is the main solid phase in the interstellar environments (F. Kemper etal., 2004), it may have important roles for the evolution of extraterrestrial organic matter. Further experiments are needed to identify the intermediate compounds as well as to observe the change in mineral phases during the reactions.

⋅Yamnashita Y. and Naraoka H. (2014) Two homologous series of alkylpyridines in Murchison meteorite. Geochemical Journal 48: 519-525.
⋅F. Kemper, W. J. Vriend, and A. G. G. M. Tielens(2004) THE ABSENCE OF CRYSTALLINE SILICATES IN THE DIFFUSE INTERSTELLAR MEDIUM. The Astrophysical Journal, 609, 826–837
⋅V. Vinogradoff, F. Duvernay, G. Danger, P. Theulé, and T. ChiavassaNew insight into the formation of hexamethylenetetramine (HMT) in interstellar and cometary ice analogs. Astoronomy& Astrophysics 530, A128