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Processes in ATmospheric and AStrochemical environments, 18-21 January 2021, (Europe/Berlin / UTC100) virtual event

第8回極域科学シンポジウム/個別セッション：[OA] 南極隕石 / はやぶさ12月5日（火）国語研究所 2階講堂The Eighth Symposium on Polar Science/Ordinary sessions: [OA] Antarctic meteorites / HayabusaTue. 5 Dec./2F Auditorium, National Institute for Japanese Language and Linguistics

第7回極域科学シンポジウム:[OA] 南極隕石/はやぶさ11月29日（火）国立極地研究所 1階交流アトリウム

The Grain Impact Analyzer and Dust Accumulator (GIADA) is an in-situ instrument devoted to measure the dynamical properties of the dust grains emitted by the comet. Using the GIADA Proto Flight Model (PFM), installed in a clean room in our laboratory, an extended calibration activity \citep{Sordini14} has been carried out taking into account the knowledge gained through the analyses of IDPs and cometary samples returned from comet 81P/Wild 2 \citep{Brownlee et al. 2006, Rotundi et al. 2014}. GIADA consists of three measurement subsystems: the Grain Detection System, an optical device measuring the optical cross-section of single grain without affecting its dynamical properties; the Impact Sensor that measures the momentum released from each grain that impacts its sensitive surface, and the Micro Balance System, a network of five Quartz Micro Balances measuring the cumulative dust deposition from different space directions \citep{DellaCorte14}. The results of the analyses on data acquired with the GIADA PFM and the comparison with calibration data acquired during the pre-launch campaign allowed us to improve GIADA performances and capabilities. We report the results of the following main activities: - definition of a correlation between the two GIADA Models, i.e. PFM and In-Flight Model on-board Rosetta; - characterization of the sub-systems performances (signal elaboration, sensitivities, space environment effects); - new calibration measurements and related curves by means of the GIADA PFM using realistic cometary dust analogues \citep{Ferrari14}. All the analyses performed during this extended calibration activity are allowing to fully characterize the dynamic parameters of the dust particles ejected by the comet 67P/Churyumov-Gerasimenko \citep{Rotundi et al. 2015, Fulle et al. 2015, Della Corte et al. 2015}.

IOP Publishing [Society Publisher] Silicon is present in interstellar dust grains, meteorites and asteroids, and to date 13 silicon-bearing molecules have been detected in the gas phase toward late-type stars or molecular clouds, including silane and silane derivatives. In this work, we have experimentally studied the interaction between atomic silicon and hydrogen under physical conditions mimicking those in the atmosphere of evolved stars. We have found that the chemistry of Si, H, and H2 efficiently produces silane (SiH4), disilane (Si2H6) and amorphous hydrogenated silicon (a-Si:H) grains. Silane has been definitely detected toward the carbon-rich star IRC +10216, while disilane has not been detected in space yet. Thus, based on our results, we propose that gas-phase reactions of atomic Si with H and H2 are a plausible source of silane in C-rich asymptotic giant branch stars, although its contribution to the total SiH4 abundance may be low in comparison with the suggested formation route by catalytic reactions on the surface of dust grains. In addition, the produced a-Si:H dust analogs decompose into SiH4 and Si2H6 at temperatures above 500 K, suggesting an additional mechanism of formation of these species in envelopes around evolved stars. We have also found that the exposure of these dust analogs to water vapor leads to the incorporation of oxygen into Si–O–Si and Si–OH groups at the expense of SiH moieties, which implies that if this kind of grain is present in the interstellar medium, it will probably be processed into silicates through the interaction with water ices covering the surface of dust grains. We thank the European Research Council for funding support under Synergy grant ERC-2013-SyG, G.A. 610256 (NANOCOSMOS). Also, we acknowledge partial support from the Spanish MINECO through grants MAT2017-85089-c2-1R, FIS2016-77726-C3-1-P, FIS2016-77578-R, AYA2016-75066-C2-1-P and RyC-2014-16277. Support from the FotoArt-CM Project (P2018/NMT 4367) through the Program of R&D activities between research groups in Technologies 2013, cofinanced by European Structural Funds, is also acknowledged. G.T.C. acknowledges funding from the Comunidad Autonoma de Madrid (PEJD-2018-PRE/IND-9029). Peerreview

13 pags., 12 figs., 2 tabs., Interstellar carbonaceous dust is mainly formed in the innermost regions of circumstellar envelopes around carbon-rich asymptotic giant branch stars (AGBs). In these highly chemically stratified regions, atomic and diatomic carbon, along with acetylene, are the most abundant species after H and CO. In a previous study, we addressed the chemistry of carbon (C and C) with H showing that acetylene and aliphatic species form efficiently in the dust formation region of carbon-rich AGBs whereas aromatics do not. Still, acetylene is known to be a key ingredient in the formation of linear polyacetylenic chains, benzene, and polycyclic aromatic hydrocarbons (PAHs), as shown by previous experiments. However, these experiments have not considered the chemistry of carbon (C and C) with CH. In this work, by employing a sufficient amount of acetylene, we investigate its gas-phase interaction with atomic and diatomic carbon. We show that the chemistry involved produces linear polyacetylenic chains, benzene, and other PAHs, which are observed with high abundances in the early evolutionary phase of planetary nebulae. More importantly, we have found a nonnegligible amount of pure and hydrogenated carbon clusters as well as aromatics with aliphatic substitutions, both being a direct consequence of the addition of atomic carbon. The incorporation of alkyl substituents into aromatics can be rationalized by a mechanism involving hydrogen abstraction followed by methyl addition. All the species detected in the gas phase are incorporated into nanometric-sized dust analogs, which consist of a complex mixture of sp, sp, and sp hydrocarbons with amorphous morphology., We thank the European Research Council for funding support under Synergy grant ERC-2013-SyG, G.A. 610256 (NANOCOSMOS). Also, partial support from the Spanish Research Agency (AEI) through grants MAT2017-85089-c2- 1R, FIS2016-77578-R, FIS2016-77726-C3-1-P, AYA2016- 75066-C2-1-P, and RyC-2014-16277 is acknowledged. Support from the FotoArt-CM Project (P2018/NMT 4367) through the Program of R&D activities between research groups in Technologies 2013, co-financed by European Structural Funds, is also acknowledged. G.TC. acknowledges funding from the Comunidad Autónoma de Madrid (PEJD-2018-PRE/ IND-9029)