各位老師，同學(xué)大家好！

應李元研究員的邀請，荷蘭阿姆斯特丹自由大學(xué)（Vrije University Amsterdam）林彥蒿訪(fǎng)問(wèn)我所，將于6月15日（周三）下午3:00，在綜合樓701會(huì )議室做學(xué)術(shù)報告。歡迎大家參加。

報告題目：Dry vs. Wet Moon

個(gè)人簡(jiǎn)介：林彥蒿，2014至今, 在荷蘭阿姆斯特丹自由大學(xué)讀博。目前主要研究方向為高溫高壓實(shí)驗巖石學(xué)，地球化學(xué)；主要的研究對象為月球。

報告內容：The Moon is thought to have been covered by a deep magma ocean shortly after its formation. Full crystallization of a Lunar Magma Ocean (LMO) has been modeled numerically on the basis of a small subset of experiments in the classic work of Snyder et al. (1992). A recent experimental study focused on partial LMO solidification (Elardo et al., 2011). Since ~2008, however, the traditional view of a dry Moon (Taylor et al., 2006) has been challenged by the identification of water in lunar pyroclastic glasses (Saal et al., 2008, 2013), lunar minerals including apatite (e.g., Saal et al., 2013; McCubbin et al., 2010a,b; Boyce et al., 2010; Greenwood et al., 2011; Hui et al., 2013; Tartese et al., 2013, 2014; Barnes et al., 2014, 2016) and melt inclusions in lunar olivine (Saal et al., 2013; Hauri et al., 2011; Chen et al., 2015). Water could therefore play an important role in the evolution of the Moon, including perhaps during the cooling and crystallization of an early lunar magma ocean (LMO). Water has been shown to greatly affect the physical and chemical properties of minerals and magmas, even at low concentrations (Sisson and Grove, 1993). Therefore, the presence of significant amounts of water in the ancient lunar interior requires a reassessment of lunar evolution models.
The aim of this work is to discuss the dry and wet LMO evolution with solidification and quantify water content in the early Moon based on high-pressure high-temperature experiments.