Exfoliation of kaolinite by urea-intercalation precursor and microwave irradiation assistance process

A type of exfoliated kaolinite was produced by urea-intercalation and original microwave irradiation assisted method. The product was investigated by Fourier transformation infrared (FT-IR) spectroscopy, X-ray diffraction (XRD), scanning electronic microscopy (SEM), Brunauer-Emmett-Teller (BET) and laser particle analysis techniques. FT-IR spectra show that NHCO molecule exists in the intercalated kaolinite. XRD analyses indicate that the kaolinite sheet-like structure was disordered after microwave irradiation. The urea decomposition process and explosion effect between the sheet-like structures of kaolinite under microwave irradiation were discussed. The SEM and BET analyses reveal that the end product is exfoliated kaolinite with thin particles and increased surface area. Size and zeta potential analyses show that the particle size distribution is between 250 nm and 550 nm with normal distribution and the particle is negatively charged. In comparison with the conventional grind method, the process adopted appears to be economic and the exfoliated kaolinite end product may display a significantly enhanced performance in industrial applications.     

3. Solar System Formation and Early Evolution: the First 100 Million Years

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.     

含铁绿柱石的改色机制研究

含铁绿柱石经γ射线辐照或特定温度热处理,可因铁价态的改变引起颜色发生相应变化。处理前后的吸收光谱和顺磁共振谱研究表明,辐作用使隧道位的Ｆｅ＾２＋氧化Ｆｅ％３＋,八一位上的Ｆｅ＾３＋还原为Ｆｅ＾２＋,热处理使隧道位及八面体位Ｆｅ＾３＋均还原为Ｆｅ＾２＋。     

紫外线诱导太平洋牡蛎雄核发育的研究

为诱导太平洋牡蛎雄核发育单倍体 ,本文研究利用紫外线诱导太平洋牡蛎雄核发育的条件。结果表明 :在强度为2 .8mW·cm-2 ·s-1的紫外线 (2 5 4nm)下分别照射 0 ,10 ,15 ,2 0 ,2 5 ,3 0 ,3 5 ,40 ,5 0 ,60 ,70和 80s后 ,照射 3 0s的卵子能够保持较高的受精率 (73 .5 % ) ;该处理组的D形幼虫发生率为 0。染色体检查结果显示此时单倍体率最高 (4 7.8% )。证明在强度为2 .8mW·cm-2 ·s-1的紫外线下照射 3 0s是获得雄核发育单倍体的适宜条件。研究还表明受精率和D形幼虫发生率随照射时间的增加而下降 ,遗传失活的卵子与正常精子受精后其胚胎发育至D形幼虫前期停止。实验中各处理组均出现非整倍体。原因可能由于紫外线对卵子染色体遗传失活的作用程度不同以及光线对DNA的修复作用。     

天然含钒金红石加热、淬火及电子辐射改性实验研究

天然含钒金红石样品经过1273K加热、淬火和高能电子辐照处理后性质发生不同程度的变化。XRD谱峰显示处理前后样品没有发生物相变化，显微IR图谱证明原样、加热、淬火样品的表面有少量吸附水存在，而辐射样品的显微IR图谱上没有检测到吸附水的吸收峰。用XPS分析比较了处理前后样品表面主要元素Ti、O和V的价态及含量，结果表明，原样经过处理后表面钒和氧的原子百分含量增加，其中淬火样品表面吸附水和钒的含量相对于原样增加最为明显，光催化活性相应较高；加热样品表面的吸附水和钒的含量比原样稍有增加，光催化活性与原样相当；电子辐射样品表面钒的原子百分含量相对原样增加不明显，而对水的吸附能力相对原样较低，光催化效率也略低。     

Retention of cosmogenic 3He in calcite

Cosmogenic ³He can be used to date a wide range of mineral phases because it is produced from all target elements and can be readily measured above atmospheric contamination. Calcite is a particularly attractive target mineral due to its natural abundance, large crystal size (>1 mm), and low He closure temperature (<70 °C), which limit non-cosmogenic ³He components (Copeland et al., 2007). However, several recent studies have shown that some calcite may not be retentive to helium, even under surface temperatures (Cros et al., 2014; Copeland et al., 2007). This study thus explores ³He retention and production in natural calcite samples at four different sites. Samples from two high elevation sites appear retentive to ³He over 10 kyr timescales, whereas two additional sites clearly suffer from diffusive loss of ³He. Step-degassing experiments suggest that diffusion in calcite is controlled by multiple diffusion domains, with an apparent activation energy of 25–27 kcal mol⁻¹. Although minor ³He loss is expected from the smallest diffusion domains, the observed kinetics cannot explain the poor retention at all sites. We thus propose that opaque (non-transparent) calcite may be more retentive due to the presence of imperfections in the crystal lattice. We conclude that ³He dating of calcite shows promise in some settings. However, because retention depends on crystallographic variability it must be evaluated on a case-by-case basis until robust criteria for retention can be identified.     

Neutron irradiation and post-irradiation annealing of rutile (TiO2−x ): effect on hydrogen incorporation and optical absorption

Neutron irradiation and post-irradiation annealing under oxidising and reducing conditions have been used to investigate H incorporation in, and the optical properties of, reduced (TiO_2−x ) rutile. Optical absorption in rutile is mainly due to a Ti³⁺ Ti⁴⁺ intervalence charge transfer effect. The main mechanism for H incorporation in rutile involves interstitial H not coupled to other defects, which has important implications for the rate of H diffusion, and possibly also on the electrical properties of rutile. Additional minor OH absorption bands in IR spectra indicate that a small amount of interstitial H is coupled to defects such as Ti³⁺ on the main octahedral site, and indicates that more than one H incorporation mechanism may operate. Concentration of oxygen vacancies has a controlling influence on the H affinity of rutile.     

Two‐dimensional model of diffusion processes around a river mouth

The steady state diffusion equation is solved for two‐dimensional flow around a point source along an infinite straight boundary. Solutions obtained are related to the observed distribution of temperature and salinity around the mouth of the Buller River, South Island, New Zealand.     

应用傅里叶变换红外光谱与紫外可见吸收光谱鉴别两类海水养殖灰色珍珠

Akoya珍珠属生物矿化有机宝玉石,该类珍珠的矿物组成与微结构分析、定性与其颜色形成属性的鉴定方法尚为缺乏。本文通过光学显微镜、紫外可见吸收光谱、傅里叶变换红外光谱、能量色散X射线荧光光谱对具有白色或灰色珠核的两类Akoya灰色珍珠的珍珠层与珠核的结构特征及显色机制、紫外吸收光谱、微量金属元素赋存特征进行了对比研究。结果表明:①灰色珍珠的珠核有白色与灰色两类,两类珍珠的直径主要分布在5～9mm,珍珠层厚度约300～500μm;②两类珍珠的珍珠层和珠核的主体矿物组成均为生物文石,且两者的珍珠层中均富Sr贫Mn。③灰色的珠核具有明显的富Mn特征,且由于辐照使得Mn元素的价态升高并使得珠核致灰色,并导致整个珍珠呈现灰色;④紫外可见吸收光谱检测中,一般而言具有白色珠核的灰色珍珠在300～400nm波段可见明显的反射带,而具有灰色珠核的灰色珍珠在400～500nm波段可见明显的反射带。两类灰色珍珠皆为海水养殖珍珠,研究表明这两类珍珠的紫外吸收光谱的差异可作为初步评判灰色系珍珠是否经辐照改色的依据之一。