利用EIA生物测试法快速定量筛选环境样品中的二噁污染物

将采集的环境样品分作 3份 ,1份用于高分辨色质联用多离子检测测定二的毒性当量浓度 TEQ,另 2份分别用 7-乙氧基 -异吩唑酮 -脱乙基酶 ( EROD)活力诱导法和酶免疫法 ( Enzyme Immuno Assay,EIA)进行生物测试 .结果表明 EIA和EROD这 2种生物试验方法均具有较好的准确性和很宽的线性范围 .比较 Micro- EROD分析结果与化学分析结果以及 EIA分析结果与化学分析结果 ,发现 Micro- EROD生物试验所测得的 TEQ值均高于化学分析法的 TEQ值

Nonlinear spectroscopy of cold atoms in diffuse laser light

The nonlinear spectroscopy of cold atoms in the diffuse laser cooling system is studied in this paper. We present the theoretical models of the recoil-induced resonances (RIR) and the electromagnetically-induced absorption (EIA) of cold atoms in diffuse laser light, and show their signals in an experiment of cooling Rb-87 atomic vapor in an integrating sphere. The theoretical results are in good agreement with the experimental ones when the light intensity distribution in the integrating sphere is considered. The differences between nonlinear spectra of cold atoms in the diffuse laser light and in the optical molasses are also discussed. (c) 2009 Optical Society of America

免疫酶标技术在植物细胞微管研究中的应用

在细胞分裂一分化过程中的微管动态是十分引人注目的。微管的动态主要包括微管蛋自的形成及微管的聚合—解聚反应。本工作利用离林条件下微管的聚合—解聚的可逆反应纯化了微管蛋白，并用以免疫家兔获得抗血清。在此基础上利用酶免疫分析法(En zy—me immunoas say EIA)来研究贝母(SiberianFritillary)培养细胞在不同激素作用下微管蛋白的含量及微管的分布，即利用免疫细胞化学法(immunocyto。chemicalvisulization)显示微管(microtubul。)以及用酶联免疫测试(Enzyme-Linked Im.munosorbent Assay)进行微管蛋白的定量。此外还进行了电镜下的免疫酶标微管定位观察，研究了细胞分裂后期细胞板形成过程中微管分布与取向。结果表明受外源激素控制的细胞的分化和脱分北状态，在形态变化之前细胞的微管骨架系统已有显著不同的表现，NAA、 I A A等生长素物质可能促进微管骨架的形成。免疫酶标技术应用于细胞超微结构的研究，丰富了电镜下可见的细胞结构，本研究为免疫酶标技术在植物细胞生物学中的应用提供了有用的资料。

A new enzyme immunoassay for PCDD/F TEQ screening in environmental samples: Comparison to micro-EROD assay and to chemical analysis

A new Enzyme ImmunoAssay (EIA) for PCDD/F TEQ measurement in extracts of environmental samples was described. The bioassay TEQ which derived from EIA and EROD were compared with each other and with results from chemical analysis. For all environmental samples, the EROD-TEQ is higher than the value from chemical analysis. However, the EIA-TEQ is much more identical with the value from chemical analysis. Our results indicate that the EIA assay is a complementary method to the EROD assay and should be useful as a rapid and sensitive screening tool for environmental samples in many situations. (C) 1999 Elsevier Science Ltd. All rights reserved

太阳活动变化对中低纬电离层的影响

With the variations of solar activity, solar EUV and X-ray radiations change over different timescales (e.g., from solar cycle variation to solar flare burst). Since solar EUV and X-ray radiations are the primary energy sources for the ionosphere, theirs variations undoubtedly produce significant and complicated effects on the ionosphere. So the variations of solar activity significantly affect the ionosphere. It is essential for both ionospheric theory and applications to study solar activity effects on the ionosphere. The study about solar activity variations of the ionosphere is an important part of the ionospheric climatology. It can enhance the understanding for the basic processes in the ionosphere, ionospheric structure and its change, ionosphere/thermosphere coupling, and so on. As for applications, people need sufficient knowledges about solar activity variations of the ionosphere in order to improve ionospheric models so that more accurate forecast for the ionospheric environments can be made. Presently, the whole image about the modalities of ionospheric solar activity variations is still unknown, and related mechanisms still cannot be well understood. This paper is about the effects of the 11-year change in solar activity to the low- and mid-latitude ionosphere. We use multi-type ionospheric observations and model to investigate solar activity effects on the electron density and ionospheric spatial structure, and we focus on discussing some related mechanisms. The main works are as follows: Firstly, solar activity variations of ionospheric peak electron density (NmF2) around 1400 LT were investigated using ionosonde observations in the 120°E sector. The result shows that the variation trend of NmF2 with F107 depends on latitudes and seasons. There is obvious saturation trend in low latitudes in all seasons; while in middle latitudes, NmF2 increases linearly with F107 in winter but saturates with F107 at higher solar activity levels in the other seasons. We calculated the photochemical equilibrium electron density to discuss the effects induced by the changes of neutral atmosphere and dynamics processes on the solar activity variations of NmF2. We found that: (1) Seasonal variation of neutral atmosphere plays an important role in the seasonal difference of the solar activity variations of NmF2 in middle latitudes. (2) Less [O]/[N2] and higher neutral temperature are important for the saturation effect in summer, and the increase of vibrational excited N2 is also important for the saturation effect. (3) Dynamics processes can significantly weaken the increase of NmF2 when solar activity enhances, which is also a necessary factor for the saturation effect. Secondly, solar activity variations of nighttime NmF2 were investigated using ionosonde observations in the 120°E sector. The result shows that the variation trends of NmF2 with F107 in nighttime are different from that in daytime in some cases, and the nighttime variation trends depend on seasons. There is linear increase trend in equinox nighttime, and saturation trend in summer nighttime, while the increase rate of NmF2 with F107 increases when solar activity enhances in winter nighttime (we term it with “amplification trend”). We discussed the possible mechanisms which affect the solar activity variations of nighttime NmF2. The primary conclusions are as follows: (1) In the equatorial ionization anomaly (EIA) crest region, the plasma influx induced by the pre-reversal enhancement (PRE) results in the change of the variation trend between NmF2 and F107 from “saturation” to “linear” after sunset in equinoxes and winter; while the recombination process at the F2-peak is the primary factor that affects the variation trend of NmF2 with F107 in middle latitudes. (2) The recombination coefficient at the F2-peak height reaches its maximum at moderate solar activity level in winter nighttime, which induces NmF2 attenuates more quickly at moderate solar activity level. This is the main reason for the amplification trend. (3) The change of the recombination process at the F2-peak with solar activity depends on the increases of neutral parameters (temperature, density et al.) and the F2-peak height (hmF2). The seasonal differences in the changes of neutral atmosphere and hmF2 with solar activity are the primary reasons for the seasonal difference in the variation trend of nighttime NmF2 with F107. Finally, we investigated the solar activity dependence of the topside ionosphere in low latitudes using ROCSAT-1 satellite (at 600 km altitude) observations. The primary results and conclusions are as follows: (1) Latitudinal distribution of the plasma density is local time, seasonal, and solar activity dependent. In daytime, there is a plasma density peak at the dip equator. The peak is obviously enhanced at high solar activity level, and the strength of the peak strongly depends on seasons. While at sunset, two profound plasma density peaks (double-peak structure) are found in solar maximum equinox months. (2) Local time dependence of the latitudinal distribution is due to the local time variation of the equatorial dynamics processes. Double-peak structure is attributed to the fountain effect induced by strong PRE. Daytime peak enhances with solar activity since the plasma density increases with solar activity more strongly at the dip equator due to the equatorial vertical drift, and its seasonal dependence is mainly due to the seasonal variations of neutral density and the equatorial vertical drift. In the sunset sector, seasonal and solar activity dependences of the latitudinal distribution are related to the seasonal and solar activity variations of PRE. (3) The variation trend of the plasma density with solar activity shows local time, seasonal, and latitudinal differences. That is different from the changeless amplification trend at the DMSP altitude (840 km). Profound saturation effect is found in the dip equator region at equinox sunset. This saturation effect in the topside ionosphere is realated to the increase of PRE with solar activity. Solar activity variation trend of the topside plasma density was discussed quantitatively by Chapman-α function. The result shows that the effect induced by the change of the scale height is dominant at high altitudes; while the variation trend of ROCSAT-1 plasma density with solar activity is suggested to be related to the changes of the peak height, the scale height, and the peak electron density with solar activity.