辽宁桓仁软玉的宝石学特征研究   总被引：1，自引：1，他引：0  

林维峰 《岩矿测试》2012,31(5):794-797

利用常规检测及薄片观察、红外光谱、化学分析法,对产自辽宁桓仁的一种灰白色玉石的矿物成分、化学成分及宝石学性质进行了较为系统的研究。测得其折射率为1.60,相对密度为3.08,摩氏硬度为6.5±。偏光显微镜下显示玉石的主要组成矿物为透闪石及普通角闪石,杂质矿物为透辉石、磷灰石、碳酸盐矿物、蛇纹石等,呈不等粒变晶结构、叶片状变晶结构及交代结构。玉石的组构特征导致其透明度较差,颜色不均匀,具黑色斑点及绿色团块状包体。红外光谱特征与标准的透闪石特征非常相近,证明该玉石为透闪石玉(软玉),其化学分析结果与和田玉及岫岩软玉结果相近。普通角闪石的存在(已黑云母化)一定程度影响了玉石的品质。  相似文献   

Mineralogical and Physical Characteristics of White Sandstone of Abu Rodeiyim Quarry (Sinai), and its Possible Industrial Utilization     

Mostafa Gouda TEMRAZ 《《地质学报》英文版》2012,86(2):440-446

Mineralogical, geochemical, and textural analyses of the white sandstones (Abu Thora Fm.) of Carboniferous in the Abu Rodeiyim region show that they are fluviomarine, well-sorted, high-purity, and high-grade silica SiO2 (average 99.56%). The results indicate that by simple treatment, the white sandstones can reach a high degree of purity, suitable for different industrial purposes (e.g. manufacture of silicon photovoltaic, crystal, and TV screens, art, and domestic and optical glass).  相似文献   

新疆、青海、俄罗斯糖白玉的宝石学特征对比分析     

张攀  刘喜锋  李竞妍  陈美华 《地质科学译丛》2011,(4):31-38

为了查明新疆、青海、俄罗斯三地所产糖白玉的结构、成分和成因差异,在观察原料外观特征的基础上,采用常规宝石学方法、偏光显微镜、X射线粉末衍射仪和电子探针研究新疆、青海、俄罗斯糖白玉样品,从结构类型、矿物组成、化学成分和成因特征等方面进行对比分析。结果表明,以上三地糖白玉的主要矿物组成均为透闪石,次要矿物组成则各有不同。新疆、俄罗斯糖白玉以毛毡状变晶结构为主,青海糖白玉以纤维状变晶结构和纤维-隐晶质变晶结构为主;初步认定以上三地糖白玉的糖色为次生色,主要由褐铁矿导致。结合相关地质背景和风化作用特征,推测以上三地糖白玉不同的外观特征主要受玉体成矿后期和成矿期结束后周围环境变化的影响。  相似文献   

The Harry Creek Deformed Zone,a retrograde schist zone of the Arunta Block,central Australia     

A. R. Allen  L. P. Black 《Australian Journal of Earth Sciences》2013,60(1-2):17-28

The Harry Creek Deformed Zone, a retrograde schist zone of epidote amphibolite facies grade, which separates the granulite facies Utralanama Block from the amphibolite facies Ankala Block in the southeastern Strangways Range, N.T., is typical of the retrograde schist zones transecting the Arunta Block. Associated with the deformed zone is a small deformed granitic pluton and its various offshoots—the Gumtree Granite Suite—which provides structural and geochrono‐logical evidence that the Harry Creek Deformed Zone has had a polyphase deforma‐tional history. Early movements within the deformed zone pre‐dated intrusion of the Gumtree Granite Suite and resulted in the movement of the Utralanama and Ankala Blocks into their present juxtaposition. Reactivation of much of the zone during the Alice Springs Orogeny brought about the schistose character of the zone and the deformation of the granitic rocks. Further minor reactivation of the zone, subsequent to the main phase of the Alice Springs Orogeny, resulted in limited development of pseudotachylytes.

The age of the granite (990 ± 13 m.y.) gives a minimum age for initiation of the zone, and evidence for the nature of the structures associated with the early movements is presented. It is suggested that the Harry Creek Deformed Zone represents a post‐orogenic wrench fault which has been reactivated. Early movements, which were of a brittle transcurrent nature, brought about major uplift (up to 10 km) to the north, and lateral movements may have been of the order of 60 km in a sinistral sense. Comparison with the Redbank Zone indicates many similarities, suggestive of a similar history.  相似文献   

Gamma-ray emission from individual classical novae     

Jordi Gómez-Gomar  Margarita Hernanz  Jordi José  & Jordi Isern 《Monthly notices of the Royal Astronomical Society》1998,296(4):913-920

Classical novae are important producers of radioactive nuclei, such as ⁷Be, ¹³N, ¹⁸F, ²²Na and ²⁶Al. The disintegration of these nuclei produces positrons (except for ⁷Be) that through annihilation with electrons produce photons of energies 511 keV and below. Furthermore, ⁷Be and ²²Na decay producing photons with energies of 478 and 1275 keV, respectively, well in the γ-ray domain. Therefore, novae are potential sources of γ-ray emission. We have developed two codes in order to analyse carefully the γ-ray emission of individual classical novae: a hydrodynamical one, which follows both the accretion and the explosion stages, and a Monte Carlo one, able to treat both production and transfer of γ-ray photons. Both codes have been coupled in order to simulate realistic explosions. The properties of γ-ray spectra and γ-ray light curves (for the continuum and for the lines at 511, 478 and 1275 keV) have been analysed, with a special emphasis on the difference between carbon–oxygen and oxygen–neon novae. Predictions of detectability of individual novae by the future SPI spectrometer on board the INTEGRAL satellite are made. Concerning ²⁶Al, its decay produces photons of 1809 keV but this occurs on a time-scale much longer than the typical time interval between nova outbursts in the Galaxy, making it undetectable in individual novae. The accumulated emission of ²⁶Al from many Galactic novae has not been modelled in this paper.  相似文献   

Magnetic field evolution in neutron stars     

A. Reisenegger 《Astronomische Nachrichten》2007,328(10):1173-1177

Neutron stars contain persistent, ordered magnetic fields that are the strongest known in the Universe. However, their magnetic fluxes are similar to those in magnetic A and B stars and white dwarfs, suggesting that flux conservation during gravitational collapse may play an important role in establishing the field, although it might also be modified substantially by early convection, differential rotation, and magnetic instabilities. The equilibrium field configuration, established within hours (at most) of the formation of the star, is likely to be roughly axisymmetric, involving both poloidal and toroidal components. The stable stratification of the neutron star matter (due to its radial composition gradient) probably plays a crucial role in holding this magnetic structure inside the star. The field can evolve on long time scales by processes that overcome the stable stratification, such as weak interactions changing the relative abundances and ambipolar diffusion of charged particles with respect to neutrons. These processes become more effective for stronger magnetic fields, thus naturally explaining the magnetic energy dissipation expected in magnetars, at the same time as the longer-lived, weaker fields in classical and millisecond pulsars. (© 2007 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

厦门中华白海豚的分布和数量   总被引：9，自引：0，他引：9  

刘文华  黄宗国 《海洋学报》2000,22(6):95-101

1994～1999年在厦门海域进行84航次中华白海豚船只跟踪和照像,记录392只次。设20个监视站,进行239个月的逐日观察,记录12624只次。整个厦门海域700km2均有中华白海豚分布,它可溯河至近淡水的河道,但不游出外海。厦门西港和同安湾口内的近岸最多,跃出海面的次数有明显的季节差异,4～5月最多。厦门海域中华白海豚数量估计不足100只,仅40只左右有确切记录。种群数量目前仍有减少趋势,因而应就地和迁地保护并举,加强对这种国家一级保护物种的保护。  相似文献   

Low- and intermediate-mass close binary evolution and the initial–final mass relation     

Zhanwen Han  Christopher A. Tout  Peter P. Eggleton 《Monthly notices of the Royal Astronomical Society》2000,319(1):215-222

Using Eggleton's stellar evolution code, we carry out 150 runs of Population I binary evolution calculations with the initial primary mass between 1 and 8 M_⊙, the initial mass ratio     between 1.1 and 4, and the onset of Roche lobe overflow (RLOF) at an early, middle or late Hertzsprung-gap stage. We assume that RLOF is conservative in the calculations, and find that the remnant mass of the primary may change by more than 40 per cent over the range of initial mass ratio or orbital period, for a given primary mass. This is contrary to the often-held belief that the remnant mass depends only on the progenitor mass if mass transfer begins in the Hertzsprung gap. We fit a formula, with an error less than 3.6 per cent, for the remnant (white dwarf) mass as a function of the initial mass M _1i of the primary, the initial mass ratio q _i and the radius of the primary at the onset of RLOF. We also find that a carbon–oxygen white dwarf with mass as low as 0.33 M_⊙ may be formed if the initial mass of the primary is around 2.5 M_⊙.  相似文献   

Galactic 1.275-MeV emission from ONe novae and its detectability by INTEGRAL/SPI     

P. Jean  M. Hernanz  J. Gómez-Gomar  J. José 《Monthly notices of the Royal Astronomical Society》2000,319(2):350-364

Models of Galactic 1.275‐MeV emission produced by the decay of the radionuclide ²²Na have been computed. Several frequency–spatial distributions of novae have been investigated using recent results of nova rates and spatial distributions of novae in our Galaxy. These models allow us to estimate the lower limit of the ²²Na mass ejected per ONe nova detectable with the future spectrometer (SPI) of the INTEGRAL observatory as a function of the frequency–spatial distribution of ONe novae in the Galaxy. Calculations using recent estimations of the expected ²²Na mass ejected per ONe nova show that the detection of the Galactic emission of 1.275‐MeV photons will be difficult with the future spectrometer of the INTEGRAL observatory, whereas the cumulative emission around the Galactic Centre has some chance of being detected during the deep survey of the central radian of the Galaxy.  相似文献   

The evolution of iron-core white dwarfs     

J. A. Panei  L. G. Althaus†  O. G. Benvenuto‡ 《Monthly notices of the Royal Astronomical Society》2000,312(3):531-539

Recent measurements by Hipparcos present observational evidence supporting the existence of some white dwarf (WD) stars with iron-rich core composition. In connection with this, the present paper is aimed at exploring the structure and evolution of iron-core WDs by means of a detailed and updated evolutionary code. In particular, we examined the evolution of the central conditions, neutrino luminosity, surface gravity, crystallization, internal luminosity profile and ages. We find that the evolution of iron-rich WDs is markedly different from that of their carbon–oxygen counterparts. In particular, cooling is strongly accelerated (up to a factor of 5 for models with pure iron composition) as compared with the standard case. Thus, if iron WDs were very numerous, some of them would have had time enough to evolve at lower luminosities than that corresponding to the fall-off in the observed WD luminosity function.  相似文献