纺织品中偶氮染料还原液内芳香胺的电喷雾电离质谱分析

在优化的条件下,用电喷雾电离质谱(ESI-MS)检测了多种纺织品中由偶氮染料还原获得的芳香胺。当毛细管温度为100℃、鞘气流速为25单位、进样流速为10μL/min、电压为5kV时,信号的总离子流强度高且较稳定。实验分析了19种致癌芳香胺标准溶液的二级质谱,获得了相应物质的特征碎片离子;在此基础上,建立了基于ESI-MS对毛巾、棉布等样品中芳香胺进行快速定性分析的方法,具有灵敏度高、特异性好、检测速度快等优点。     

SporadicE ionization associated with meteor events

Two meteor events which were sighted in the Gujarat skies of India, were accompained by the visibility of sporadicE ionization on the ionograms recorded at Ahmedabad (Geog. Lat. 23·2°N, long. 72·30°E). The first event was the Dhajala fireball which flashed into the geoatmosphere along an E-N to W-S trail at about 20·40 h IST on 28 January 1976; the closest distance of the ground projection of meteor trail from Ahmedabad was 50km. The other event was a possible meteor group sighted over Ahmedabad on 28 May 1978, at about 21·10 h IST. This work describes the nature of the sporadicE ionization observed on Ahmedabad ionograms during the two events. Features of theEs echo during the Dhajala event which indicate that it could be of meteoric origin are discussed. Meteor theory is used to relate the observed ionization with the physical dimensions of the Dhajala meteorite as obtained by other workers.     

高温热水孔逸出气氡观测实验研究

本文通过在漳州龙师１＃井开展的逸出气氡观测实验研究，认为逸出气氡作为新的地震前兆观测项目是可行的，可以进行平行样观测，同时可得到Ｒｎ气／Ｒｎ水比值，作为研究地下流体前兆的一个新的参数。并对应用电离法测量逸出气氡的连续自记观测技术进行了预研究试验。     

高精度热电离质谱(TIMS)铀系法洞穴沉积物(石笋)年龄的研究

用高精度热电离质谱技术测定石笋的年龄,初步建立了热电离质谱铀系年龄的方法。 4个样品的测定结果复现性较好,铀含量、同位素比值及年龄值与标准值吻合,数据的精度大大提高,显示了质谱铀系年龄方法具有样品量少、时间短、精度高的优点。     

中国南方存在印支期的油气藏——Re-Os同位素体系的制约

利用Re-Os同位素方法开展富含有机质的沥青、原油等的研究,是确定油气成藏时间和破坏时间有效的但极富挑战性的新途径,在国内尚无研究实例报道。以我国南方最大的古油藏之一的麻江古油藏中的沥青为主要对象,采用Re-Os同位素方法试图限定油气的成藏时间和破坏时间。研究表明,麻江古油藏的固体沥青Re、Os同位素质量分数分别在41.5×10-6～642×10-6和0.21×10-6～12.15×10-6之间,N(187Re)/N(188Os)比值较高,且变化范围较大,在270.90～4074.99之间,Os同位素组成指示中等放射成因,其N(187Os)/N(188Os)比值在0.3400～3.6557之间变化。所有沥青样品的模式年龄在28～144Ma之间变化,集中在85Ma左右。通过沥青Re-Os同位素研究,结合详细地质资料,认为麻江古油藏的成藏时间为印支期—早燕山期(144Ma之前),而油藏破坏时间为燕山晚期即85Ma左右。     

超微量钐同位素的热表面电离质谱分析

采用双带测量方式,法拉第杯和离子计数器同时接收与跳峰接收相结合,建立了超微量钐同位素的热表面电离质谱的测量方法。优化了制样程序和质谱测量程序,研究了蒸发带电流对离子流强度的影响,考察了从纳克至微克不同样品用量的测量效果及其中Nd、Eu干扰核素的情况。对4 ng~2μg的天然丰度钐样品进行了同位素比值分析,相对标准偏差均小于1.1%。     

In situ U–Pb SIMS (IN-SIMS) micro-baddeleyite dating of mafic rocks: Method with examples

An in situ U–Pb SIMS (IN-SIMS) method to date micro-baddeleyite crystals as small as 3 μm is presented with results from three samples that span a variety of ages and geologic settings. The method complements ID-TIMS geochronology by extending the range of dateable crystals to sizes smaller than can be recovered by physical separation. X-ray mapping and BSE imaging are used to locate target grains in thin section, followed by SIMS analysis on a CAMECA ims 1270, using the field aperture in the transfer column to screen out ions from host phases. Internal age precisions for the method are anticipated to range from 0.1% for Precambrian rocks to 3–7% for Phanerozoic rocks. Results establish a 2689 ± 5 Ma age for mafic dikes in the Wyoming craton, USA, a 1540 ± 30 Ma age for a subaerial lava flow from the Thelon Basin of northern Canada, and a 457 ± 34 Ma age for mafic dikes in the platform sequence of southeastern Siberia. The method is ideal for relatively non-destructive dating of small samples such as extraterrestrial rocks and precious terrestrial samples.     

边缘耀斑中HeI 10830的加宽计算

讨论了 ＨｅＩ １０８３０Ａ的 Ｄｏｐｐｌｅｒ和 Ｓｔａｒｋ加宽机制以及各种加宽参数的计算，并 得到以下一些结论：辐射阻尼对 ＨｅＩ １０８３０ Ａ的加宽作用与 Ｄｏｐｐｌｅｒ效应相比可以忽略； 在公认的耀斑电子密度（Ｎｅ＝３．２ ×１０１３ｃｍ－３）的情况下，所有阻尼项均不可能产生可以 觉察的加宽；直到 Ｎｅ＝１０１５ｃｍ－３，各种阻尼对线心半宽的增加都不起作用，其值最多 在１０－３的量级，因此；线心都可以看作是Ｄｏｐｐｌｅｒ加宽；当 Ｎｅ＞１０１４ ｃｍ－３时，Ｓｔａｒｋ 加宽，特别是电子碰撞的 Ｓｔａｒｋ加宽将在 ＨｅＩ １０８３０ Ａ的加宽中起主要作用；如要 Ｓｔａｒｋ 加宽谱线的线翼比纯Ｄｏｐｐｌｅｒ加宽大１－２倍，则阻尼加宽半宽与。可以相比拟；如果 用 Ｓｔａｒｋ加宽来解释 １９８９年边缘耀斑的观测轮廓，则电子密度将达１０～（１７）ｃｍ－３，与氦 原子的碰撞阻尼（γ３）造成的加宽对Ｉ１２和Ｉ３两分量明显不同，它们对Ｉ１２的影响比对Ｉ３ 的影响大近一个量级，我们的观测显示Ｉ１２和Ｉ３线翼的延伸基本一样，因而我们的观测 轮廓不可能是γ３造成的     

The hyperthermal ionization and high absolutemeteor velocities observed with HPLA radars

High Power Large Aperture (HPLA) radars generally observe very high meteor velocities averaging over 50 km s⁻¹. There are only a few events recorded around 30 km s⁻¹, while meteors at 20 km s⁻¹ or slower are very rare. This is a clear and debated contradiction to specular meteor radar results. A high plasma density condition contributes, but the dominating phenomenon is the hyperthermal ionization mechanism due to chemical dynamics of the ionization process. The observed high velocities can be explained in terms of high hyperthermal ionization cross-sections for collisions between ablated meteoroid metal atoms such as Na and/or Fe and atmospheric species.     

The generation of ionization-shock front oscillations by a variable radiation flux

The effect of a time-varying radiation flux incident on an ionization front on the generation of ionization-shock front oscillations in the interstellar medium is analyzed analytically and numerically. We take into account both variations in the flux of ionizing radiation directly from the source that produces the ionization front and the absorption of energetic photons by the post-front plasma. Based on our calculations, we show that the time dependence of the radiation flux can be an additional factor (apart from small inhomogeneities in the interstellar medium) that contributes to the amplification of oscillations and to the kinetic energy input to the observed turbulent motions in H II regions.