复杂背景下被动FTIS定量遥感污染云团光谱

本文提出复杂背景下定量遥感污染云团光谱的算法。利用被动傅里叶变换红外光谱仪（ＦＴＩＳ）遥测目标气体和背景光谱数据及最小平方误差拟合方法,成功地解决了探测目标气体柱数密度和目标气体等效辐射温度。该处理方法不仅可用于特定污染云团的定量处理,而且可用于多种污染地区如发电厂、机场、城市交叉路口、垃圾处理站等对ＣＯ,ＣＯ２,ＮＯ,ＮＯ２,Ｎ２Ｏ,ＮＨ３,ＣＨ４,ＳＯ２,Ｈ２Ｏ,ＨＣＩ和ＨＣＨＯ等气体浓度的监测。最后,详细讨论了用该算法对模拟剂的处理结果。     

汤阴地堑及邻区的壳幔结构与地震危险性

本文利用荷泽－林县－长治剖面西段和郑州－济南剖面南段深地震测深资料,通过一、二维计算与解释,获得了汤阴地堑及邻区的二维速度结构。结果显示：该区地壳上地幔结构在纵、横向上均具明显的差异,地壳厚度变化大局部存在低速块体,对应汤阴地堑为Ｍ面隆起,隆起高点Ｍ面埋深为３１ｋｍ,向东往浚县隆起区Ｍ面逐渐加深３２ｋｍ,向西往太行山前隆起Ｍ面为一陡变带,至长治附近Ｍ面埋深增至４０ｋｍ。根据华北地区历史地震与深部结     

垦西特稠油化学降粘机理的研究

详细研究了胜利油田垦西特稠油中的胶质、沥青质用降粘剂处理前后的红外特征吸收峰和透射电镜照片的变化。由红外光谱数据和透射电镜分析可知,降粘剂分子借助强的形成氢键的能力和渗透、分散作用进入胶质和沥青质片状分子之间,破坏了胶质、沥青质分子平面重叠的聚集体,使聚集结构变得疏松,表明聚集有序性降低是稠油降粘的主要机理。     

天文用近红外焦平面阵列

总结了天文用红外焦平面阵列（IRFPA）的发展历程,阐述了IRFPA的结构,重点介绍了InSb、HgCdTe和Ptsi三种近红外探测器阵列,结合目前正在筹建的红外太阳塔计划,对其各项性能指标作了详细比较．     

12-μm fine-structure emission line and continuum images of G333.6–0.2

We present high spatial resolution (∼0.8 arcsec) diffraction-limited 12.8-μm Ne  ii fine-structure emission line and 12.5-μm continuum images of the bright southern compact H  ii region G333.6–0.2, taken with the mid-infrared imaging polarimeter NIMPOL. The two images show remarkably similar, compact, yet asymmetric, flux distributions. The [Ne  ii ] image shows a complex structure near the ionizing source(s) which we interpret in terms of the ionization structure of the H  ii region. It is found that G333.6–0.2 is more likely to be excited by a cluster of O and B stars than by a single star.     

贵州含钾粘土岩及其活化产物的红外光谱

根据红外光谱测试结果,贵州含钾粘土岩可分成两类。一类的主要含钾矿物为伊利石,另一类是富镁1M型伊利石;其他主要组成矿物为石英和高岭石等。这两类岩石加热时有相似的变化行为。遵义含钾粘土岩活化产物的红外光谱为开发利用含钾粘土岩正确选择活化剂和设计活化工艺、探讨钾的活化机理提供了试验资料。     

电偶源频率电磁测深中的EX分量

在电偶源频率电磁测深的各场量中,电场ＥＸ分量具有分辨率同,观测信噪比高,不需作近场改正等优点。在有地表电性不均匀引起的静态偏移情况下,可通过转换相位消除静态偏移。因此在资料处理与解释中可不局限于比值电阻率的模式,使频率电磁测深具有更大的灵活性与适应性。     

硅酸盐碳星的红外观测及能谱分布

本文对赤纬负10°以北的所有11颗硅酸盐碳星进行了近红外JHK观测．结合可见波段及红外天文卫星的观测结果,讨论了它们的红外双色图及能谱分布,并将其与正常碳星的结果相比较,进而讨论了它们的演化状态．     

Timing properties of the X-ray pulsar EXO 2030+375 during an X-ray outburst

We present Rossi X-ray Timing Explorer ( RXTE ) observations of the Be/X-ray transient EXO 2030+375 during an outburst after a period of quiescence between 1993 August and 1996 April. When active, EXO 2030+375 is normally detected at each periastron passage of the neutron star. Our observations correspond to the third periastron passage after the source 'turned on' again. All outbursts after the quiescent period, including the one reported here, have been occurring at a much earlier binary phase than in the past. We discuss the possible mechanisms that may explain this shift in the onset of the outburst. Pulsations in the X-ray radiation are detected throughout the entire run. The neutron star spun up during the outburst at a rate of −1.16×10⁻⁸ s s⁻¹, but no variations in the shape of the pulse profile as a function of intensity were seen. A correlation between the hardness ratio and the intensity is observed at low energies (6–12/2–6 keV). By comparing the magnetospheric and corotation radii we argue that the neutron star spins at a rate close to the equilibrium period. Finally, we perform pulse-phase spectroscopy and comment on changes seen as a function of spin phase.     

K-band polarimetry of seven high-redshift radio galaxies

We present the results of K -band imaging polarimetry of seven 3CR radio galaxies with 0.7 <  z  < 1.2. We find strong evidence for polarization in three sources: 3C 22, 3C 41 and 3C 114. Of these, 3C 41 shows strong evidence of having a quasar core the infrared light of which is scattered by dust. We also find some evidence for polarization in 3C 54 and in 3C 356. The two point-like sources (3C 22 and 3C 41) and the barely-elongated 3C 54 appear to have of order 10 per cent of their K -band flux contributed by scattered light from the active nucleus. We conclude that scattered nuclear light can form a significant component of the near-infrared light emitted by high-redshift radio galaxies, and discuss models in which the scattering particles are electrons and dust grains.