日本地球惑星科学連合2016年大会

講演情報

ポスター発表

セッション記号 P (宇宙惑星科学) » P-PS 惑星科学

[P-PS14] 宇宙における物質の形成と進化

2016年5月25日(水) 17:15 〜 18:30 ポスター会場 (国際展示場 6ホール)

コンビーナ:*橘 省吾(北海道大学大学院理学研究院自然史科学専攻地球惑星システム科学分野)、三浦 均(名古屋市立大学大学院システム自然科学研究科)、大坪 貴文(東京大学大学院総合文化研究科)

17:15 〜 18:30

[PPS14-P07] アンモニアのモンモリロナイト及びサポナイトへの吸着・脱着に伴う窒素同位体分別

*菅原 春菜1高野 淑識1小川 奈々子1力石 嘉人1大河内 直彦1 (1.海洋研究開発機構)

キーワード:窒素同位体分別、吸着、アンモニア、星間分子雲、粒子表面化学

Solar system objects show wide variation in the nitrogen isotopic composition. The δ15N value (‰, normalized as vs. Air) ranges from -400‰ in the solar wind [1] and Jovian atmosphere [2] to around +1500‰ of comets, chondrites, and interplanetary dust particles (IDPs)[3, 4]. These pristine solar system materials also show occasional extreme 15N-enrichment up to +5000‰ [5, 6]. This δ15N variation in the solar system objects is considered to have been inherited from the cold interstellar environments [7]. However, only a few models can explain the interstellar chemistry to enhance 15N-enrichments, such as photodissociation of nitrogen molecules and subsequent formation of ammonia [8], and conceivable isotopic fractionation processes have not well understood.
In the study, we conducted simple adsorption-desorption experiments using ammonia gas and two clay minerals (montmorillonite and saponite). From the results, we propose the adsorption-desorption process of ammonia on grain surface of interstellar dusts as a potential mechanism for 15N-enrichmentin interstellar environments. Ammonia is a simple nitrogen-containing molecule and one of major nitrogen carriers in the molecular clouds. It is a highly reactive chemical and regarded as a precursor for other complex nitrogen-containing molecules. Thus, adsorption of ammonia could be a first step for grain surface chemistry to form more complex organic molecules. The adsorption-desorption experiments were performed to examine the possibility of nitrogen isotopic fractionation of ammonia by adsorption and desorption on the clay minerals. Each clay mineral sample, with controlled amount of water (0, 5, 10, 20 wt.% vs. dry cry minerals), was sealed into the glass serum bottles with ammonia gas (+27‰, SI Science). The glass vial was rested for a week under room temperature (25℃) to reach a stable state before analysis. After the initial analysis was completed, the glass vial was vacuumed for 1 to 8 hours to examine the results under vacuumed environment. The nitrogen isotopic composition of the adsorbed ammonia at each step of the experiments was determined by nanoEA/IRMS technique [9].
The results showed that adsorbed ammonia generally had larger δ15N value than the initial ammonia gas. The degree of isotopic fractionation from the initial ammonia were +2.4~+40.3‰ for montmorillonite and -1.6~44.4‰ for saponite as Δ15N value. There was also a negative correlation observed between the adsorbed ratio (wt. %) and the δ15N value. When the glass vial was vacuumed for only 1 hour, the δ15N of the remaining ammonia increased (+64.1‰ for montmorillonite and +60.1‰ for saponite as Δ15N value). However, when the glass vial was vacuumed more than 1 hour, selective removal of 15NH3 was observed. The water content of the sample was not an influential factor throughout the experiments. The results suggest that adsorption and desorption of ammonia on clay minerals causes significant nitrogen isotopic fractionation (Δ15N=−1.6~+64.1‰) and could be a potential mechanism for 15N-enrichment in interstellar environments.
Reference: [1] Marty B. et al. (2011) Science 332, 1533. [2] Abbas M. M. et al. (2004) APJ 602, 1063 [3] Bonal L. et al. (2010) GCA 74, 6590. [4] Manfroid J. et al. (2009) A&A 503, 613. [5] Briani G. et al. (2009) PNAS 106, 105222. [6] Hashiguchi M. et al. (2015) Geochem. J. 49, 377. [7] Rogers S. D. & Charnley S. B. (2008) Mon. Not. R. Astron. Soc. 385, L48. [8] Chakraborty S. et al. (2014) PNAS 111, 14704. [9] Ogawa N. O. et al. (2010) in Earth, Life, and Isotopes. pp.339.