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91.
偏岭石及煅烧高岭石的红外光谱研究 总被引:3,自引:0,他引:3
通过对偏岭石和相应煅烧高岭石的红外光谱测定,发现偏岭石同煅烧高岭石在结构上有很大的差异。在偏岭石中不存在非晶态SiO_2相,其中Si—O_4四面体同Al—O_6八面体是相互聚合的:煅烧高岭石(600~995℃)中则不同,其中Si大部分是以独立的非晶态SiO_2相存在,而同其中的Al_2O_3相分离。偏岭石同煅烧高岭石的关系是:对偏岭石进行一定温度的煅烧,它可以转变成像煅烧高岭石一样的结构状态。 相似文献
92.
石膏热学性质的实验研究 总被引:2,自引:0,他引:2
用差示扫描1热仪测定石膏(CaSO_4·2H2O)的脱水活化能;用红外光谱仪研究掺入微量Eu ̄(3+),Mn ̄(2+),Pb ̄(2+)后,在不同温度煅烧下产物的红外光谱图,并测定其热发光性质;对石膏以及掺杂后的热学性质进行了讨论。 相似文献
93.
霞石正长岩是重要的炼铝资源和陶瓷、玻璃原料。文中利用扫描电镜、X衍射、红外线、电子探针等,综合分析方法对黑英山霞石正长岩的矿物学特征作了详细研究。着重描述了岩石的矿物组合、矿物生成及变化特征。对主要矿物进行了化学成分及X衍射分析,测得霞石成分:SiO_243.66%,Al_2O_330.97%,K_2O4.23%,Na_2O18.46%(Na_2O高于其它地区的霞石)。根据霞石单矿物实测成分计算出其晶体化学分子式为:(K_(0.525)Na_(3.528)Ca_(0.012))_(4.065)[Cr_(0.010)Al-(3.559)Mg_(0.009)Fe_(0.054)Mn_(0.012)Ti_(0.008)Si_(4.258)O_(16)];测得霞石的主要X衍射d值为:0.302~0.303,0.386~0.389,0.1388~0.1391(nm)。测得微斜长石的成分:SiO_264.82%,Al_2O_319.68%,K_2O11.77%,Na_2O2.30%,求得其三斜度△=0.83~1.00,属低微斜长石。通过霞石正长岩中钾长石与霞石矿物中对K原子分配值计算和作图,解得矿物生成温度为400~500℃。测得岩石中的钠长石主要为低钠长石,属后期交代矿物。 相似文献
94.
The remote sensing observational study for infrared radiation of rocks was proceeded during the loading on rocks until failure.
The major instruments used in experiments were transient spectrum apparatus, intelligent spectrum apparatus, infrared radiation
thermometer, infrared spectrum radiometer, and infrared thermal imaging system. The experiments for 26 kinds of rocks were
made. The studies show that infrared radiation temperature of rocks increases along with increasing of stress. The amplitude
of infrared radiation spectrum of rocks also increases along with increasing of stress. The observational results of infrared
thermal imaging of rocks are consistent with infrared radiation temperature. Before formation of major faults for some rocks,
the belt-shape thermal imaging of temperature anomaly displaies in position of future major faults. This study has led the
new technology of remote sensing into rock mechanics and tend to establish a new field in rock mechanics — remote sensing
rock mechanics (or remote sensing rock physics). The application of remote sensing rock mechanics in prediction of earthquake
and rock burst, and in measurement of stress field in rock mass is expected.
The Chinese version of this paper appeared in the Chinese edition ofActa Seismologica Sinica,14, Supp., 645–652, 1992.
Jin-Shen HAO, Ji-Han LI, Xiao-Hong LIU, Yi-Qiao ZHI, Jin-Kai ZHANG, Yong-Hong Lü, Yi LIU, Yun-Shen YU, He ZHANG, Quan-Quan
JI, Xiao-Fan ZHU and Ning CHEN took part in this work.
This subject is supported by the Chinese Joint Seismological Science Foundation (91006).
Work of Institute of Geophysics, SSB (93A0009). 相似文献
95.
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98.
Nathan Roche Steve Eales & Hans Hippelein 《Monthly notices of the Royal Astronomical Society》1998,295(4):946-958
We investigate the angular correlation function, ο(θ), of the galaxies detected in the 2.1-μm K ' band in 17 fields (101.5 arcmin2 in total), each containing a z ∼1.1 radio galaxy. There is a significant detection of galaxy clustering at a limit of K ∼20, with a ο(θ) amplitude similar to that estimated by Carlberg et al. at K =21.5. The ο(θ) amplitudes of these K -limited samples are higher than expected from the faint galaxy clustering in the blue and red passbands, but consistent with a pure luminosity evolution model if clustering is stable (ε=0) and the correlation function of early-type galaxies is steeper than that of spirals.
We do not detect a significant cross-correlation between the radio galaxies and the other galaxies in these fields. The upper limits on the cross-correlation are consistent with a mean clustering environment of Abell class 0 for z ∼1.1 radio galaxies, similar to that observed for radio galaxies at z ∼0.5, but would argue against an Abell class 1 or richer environment. As Abell 0 clustering around the radio galaxies would not significantly increase the ο(θ) amplitude of galaxies in these fields, stable clustering with a steep ξ( r ) for E/S0 galaxies appears to remain the most likely interpretation of the ο(θ) amplitude.
At K ≤20, the number of galaxy–galaxy pairs of 2–3 arcsec separation exceeds the random expectation by a factor of 2.15±0.26. The excess of close pairs is comparable to that previously reported for R -band data, and consistent with a ∼(1+ z )2 evolution of the galaxy merger rate. 相似文献
We do not detect a significant cross-correlation between the radio galaxies and the other galaxies in these fields. The upper limits on the cross-correlation are consistent with a mean clustering environment of Abell class 0 for z ∼1.1 radio galaxies, similar to that observed for radio galaxies at z ∼0.5, but would argue against an Abell class 1 or richer environment. As Abell 0 clustering around the radio galaxies would not significantly increase the ο(θ) amplitude of galaxies in these fields, stable clustering with a steep ξ( r ) for E/S0 galaxies appears to remain the most likely interpretation of the ο(θ) amplitude.
At K ≤20, the number of galaxy–galaxy pairs of 2–3 arcsec separation exceeds the random expectation by a factor of 2.15±0.26. The excess of close pairs is comparable to that previously reported for R -band data, and consistent with a ∼(1+ z )
99.
Chandrasekhar T. Ashok N. M. Tej Anandamayee Mondal Soumen Watson P. V. 《Earth, Moon, and Planets》1998,81(2):111-121
During the recent apparition of comet Hale—Bopp (1995 O1) near infrared photometric observations were carried out in the J,
H, K filter bands and also in the 3.0—3.4 μm region at the 1.2 m telescope at Gurushikkar, India. The effective temperature
of the comet was substantially higher than the equilibrium blackbody temperature. A mean superheat value of 1.83 was derived
in the post-perihelion phase which implies that a large fraction of the grain population are made up of small and hot grains
with radii <0.5 μm. High albedo values of ∼0.4 were also derived in the scattering angle range 135° to 160° which could explain
the unusual brightness of comet Hale—Bopp.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
100.
We exclude hydrogen-burning stars, of any mass above the hydrogen-burning limit and any metallicity, as significant contributors to the massive haloes deduced from rotation curves to dominate the outer parts of spiral galaxies. We present and analyse images of four nearly edge-on bulgeless spiral galaxies (UGC 711, NGC 2915, UGC 12426, UGC 1459) obtained with ISOCAM (The CAMera instrument on board the Infrared Space Observatory ) at 14.5 and 6.75 μm. Our sensitivity limit for detection of any diffuse infrared emission associated with the dark haloes in these galaxies is a few tens of μJy per 6 × 6 arcsec2 pixel, with this limit currently set by remaining difficulties in modelling the non-linear behaviour of the detectors. All four galaxies show zero detected signal from extended non-disc emission, consistent with zero halo-like luminosity density distribution. The 95 per cent upper limit on any emission, for NGC 2915 in particular, allows us to exclude very low mass main-sequence stars ( M > 0.08 M⊙) and young brown dwarfs (≲1 Gyr) as significant contributors to dark matter in galactic haloes. Combining our results with those of the Galactic microlensing surveys, which exclude objects with M < 0.01 M⊙, excludes almost the entire possible mass range of compact baryonic objects from contributing to Galactic dark matter. 相似文献