论文标题
在室温下辉石（晶链硅酸盐）的红外光谱
Infrared Spectra of Pyroxenes (Crystalline Chain Silicates) at Room Temperature
论文作者
论文摘要
辉石晶体在陨石中很常见，但在天文环境中很少有成分。我们提出了17 mg--fe-和含有ca的邻苯二烯的定量室温光谱，以及CA-甲状腺素的含量，以辨别趋势，以识别晶体结构和广泛组成的趋势。数据是使用钻石砧细胞产生的：我们的条带强度比在KBR或聚乙烯分散体中测得的频带强度高6倍，其中包括路径长度（来自晶粒尺寸）和数据处理中未解决的表面反射的变化。 Pyroxenes具有多样的光谱：只有两个频段，即10.22〜 $μ$ m和15.34〜 $μ$ m的Enstatite（EN $ _ {99} $），都是所有人的共同点。峰值波长通常会随着Ca或Fe取代而增加。然而，随着Fe成分从0增加到60％，MGFE-碳烯中的两个频段转移到较短的波长。一个高强度带的从11.6〜 $μ$ m转移到11.2〜 $μ$ m，并且随着Fe增加到每 / 〜Cent的100〜;它类似于通常用橄榄石或玻璃石的天文特征。 13至和16〜 $μ$ m之间的独特辉石带显示了它们在JWST获得的Miri光谱中的识别方面的希望。如果使用拟议的Spica望远镜获得数据，则可以诊断出40至80〜 $μ$ m之间的许多辉石带。我们的数据表明，在波长$ \ gtrsim 28〜μ $ m处的室温实验室和冷$ \ sim 10-k $天文尘埃特征之间的比较可以导致（mg，fe） - pyroxenes-含有7--15％的fe-fe- pyroxenes，而不是它们的真实价值少，因为某些温度变化了一些含糊不清的变化。因此，某些天文学硅酸盐可能包含比以前想象的更多的Fe，更少的Mg。
Pyroxene crystals are common in meteorites but few compositions have been recognized in astronomical environments. We present quantitative room-temperature spectra of 17 Mg-- Fe-- and Ca--bearing ortho- and clinopyroxenes, and a Ca-pyroxenoid in order to discern trends indicative of crystal structure and a wide range of composition. Data are produced using a Diamond Anvil Cell: our band strengths are up to 6 times higher than those measured in KBr or polyethylene dispersions, which include variations in path length (from grain size) and surface reflections that are not addressed in data processing. Pyroxenes have varied spectra: only two bands, at 10.22~$μ$m and 15.34~$μ$m in enstatite (En$_{99}$), are common to all. Peak-wavelengths generally increase as Mg is replaced by Ca or Fe. However, two bands in MgFe-pyroxenes shift to shorter wavelengths as the Fe component increases from 0 to 60 per cent. A high-intensity band shifts from 11.6~$μ$m to 11.2~$μ$m and remains at 11.2~$μ$m as Fe increases to 100~per~cent; it resembles an astronomical feature normally identified with olivine or forsterite. The distinctive pyroxene bands between 13~ and 16~$μ$m show promise for their identification in MIRI spectra obtained with JWST. The many pyroxene bands between 40 and 80~$μ$m could be diagnositic of silicate mineralogy if data were obtained with the proposed SPICA telescope. Our data indicate that comparison between room-temperature laboratory bands for enstatite and cold $\sim 10-K$ astronomical dust features at wavelengths $\gtrsim 28~μ$m can result in the identification of (Mg,Fe)- pyroxenes that contain 7--15 % less Fe-- than their true values because some temperature shifts mimic some compositional shifts. Therefore some astronomical silicates may contain more Fe, and less Mg, than previously thought.
