Geological,fluid inclusion and stable isotope studies of Mo mineralization,Galway Granite,Ireland     

V. Gallagher  M. Feely  H. Högelsberger  G. R. T. Jenkin  A. E. Fallick 《Mineralium Deposita》1992,27(4):314-325

Mo mineralization within the Galway Granite at Mace Head and Murvey, Connemara, western Ireland, has many features of classic porphyry Mo deposits including a chemically evolved I-type granite host, associated K- and Si-rich alteration, quartz vein(Mace Head) and granite-hosted (Murvey) molybdenite, chalcopyrite, pyrite and magnetite mineralization and a gangue assemblage which includes quartz, muscovite and K-feldspar. Most fluid inclusions in quartz veins homogenize in the range 100–350°C and have a salinity of 1–13 eq. wt.% NaCl. They display Th-salinity covariation consistent with a hypothesis of dilution of magmatic water by influx of meteoric water. CO₂-bearing inclusions in an intensely mineralized vein at Mace Head provide an estimated minimum trapping temperature and pressure for the mineralizing fluid of 355°C and 1.2 kb and are interpreted to represent a H₂O-CO₂ fluid, weakly enriched in Mo, produced in a magma chamber by decompression-activated unmixing from a dense Mo-bearing NaCl-H₂O-CO₂ fluid. ³⁴S values of most sulphides range from c. 0 at Murvey to 3–4 at Mace Head and are consistent with a magmatic origin. Most quartz vein samples have ¹⁸O of 9–10.3 and were precipitated from a hydrothermal fluid with ¹⁸O of 4.6–6.7. Some have ¹⁸O of 6–7 and reflect introduction of meteoric water along vein margins. Quartz-muscovite oxygen isotope geothermometry combined with fluid inclusion data indicate precipitation of mineralized veins in the temperature range 360–450°C and between 1 and 2 kb. Whole rock granite samples display a clear ¹⁸O-D trend towards the composition of Connemara meteoric waters. The mineralization is interpreted as having been produced by highlyfractionated granite magma; meteoric water interaction postdates the main mineralizing event. The differences between the Mace Head and Murvey mineralizations reflect trapping of migrating mineralizing fluid in structural traps at Mace Head and precipitation of mineralization in the granite itself at Murvey.  相似文献   

An exact solution of the equation of transfer with three-term scattering indicatrix in an exponential atmosphere     

S. Karanjai  T. K. Deb 《Astrophysics and Space Science》1991,179(1):89-96

The general equation for radiative transfer in the Milne-Eddington model is considered here. The scattering function is assumed to be quadratically anisotropic in the cosine of the scattering angle and Planck's intensity function is assumed for thermal emission. Here we have taken Planck's function as a nonlinear function of optical depth, viz.,B _v(T)=b _o+b ₁ e ^–. The exact solution for emergent intensity from the bounding face is obtained by the method of the Laplace transform in combination with the Wiener-Hopf technique.  相似文献   

Geology and tectonics of the Themis Regio-Lavinia Planitia-Alpha Regio-Lada Terra area,Venus: Results from Arecibo image data     

D. A. Senske  D. B. Campbell  J. W. Head  P. C. Fisher  A. A. Hine  A. deCharon  S. L. Frank  S. T. Keddie  K. M. Roberts  E. R. Stofan  J. C. Aubele  L. S. Crumpler  N. Stacy 《Earth, Moon, and Planets》1991,55(2):97-161

New radar images obtained from the Arecibo Observatory (resolution 1.5–4.0 km) for portions of the southern hemisphere of Venus show that: the upland of Phoebe Regio contains the southern extension of Devana Chasma, a rift zone extending 4200 km south from Theia Mons and interpreted as a zone of extension; Alpha Regio, the only large region of tessera within the imaged area, is similar to tessera mapped elsewhere on the planet and covers a smaller percentage of the surface than that observed in the northern high latitudes; the upland made of Ushas, Innini and Hathor Montes consists of three distinct volcanic constructs; Themis Regio is mapped as an ovoid chain of radar-bright arcuate single and double ring structures, edifices and bright lineaments. This area is interpreted as a region of mantle upwelling and on the basis of apparent split and separated features, a zone of localized faulting and extension. Linear zones of deformation in Lavinia Planitia are characterized by lineament belts that are often locally elevated, are similar to ridge belts mapped in the northern high latitudes and are interpreted to be characterized mainly by compression; radar-bright lava complexes within Lavinia Planitia are unique to this part of the planet and are interpreted to represent areas of eruption of high volumes of extremely fluid lava; the upland of Lada Terra is bound to the north by a linear deformation zone interpreted as extensional, is characterized by large ovoids and coronae, is interpreted to be associated with an area of mantle upwelling, and is in contrast to the northern high latitude highland of Ishtar Terra. Regions of plains in the southern hemisphere cover about 78%; of the mapped area and are interpreted to be volcanic in origin. Located within the area imaged (10–78 S) are 52 craters interpreted to be of impact origin ranging from 8 to 157 km in diameter. On the basis of an overall crater density of 0.94 craters/10⁶ km², it is determined that the age of this part of the Venus surface is similar to the 0.3 to 1.0 billion year age calculated for the equatorial region and northern high latitudes. The geologic characteristics of the portion of the Venus southern hemisphere imaged by Arecibo are generally similar to those mapped elsewhere on the planet. This part of the planet is characterized by widespread volcanic plains, large volcanic edifices, and zones of linear belt deformation. The southern hemisphere of Venus differs from northern high latitudes in that tessera makes up only a small percentage of the surface area and the ovoid chain in Themis Regio is unique to this part of the planet. On the basis of the analysis presented here, the southern hemisphere of Venus is interpreted to be characterized by regions of mantle upwelling on a variety of scales (ovoids, region made up of Ushas, Innini and Hathor Montes), upwelling and extension (Themis Regio) and localized compression (lineament belts in Lavinia Planitia).  相似文献   

Exact solution of the equation of transfer in a finite exponential atmosphere by the method of laplace transform and linear singular operators     

S. Karanjai  T. K. Deb 《Astrophysics and Space Science》1991,181(2):267-275

An approximate solution of the transfer equation for coherent scattering in stellar atmospheres with Planck's function as a nonlinear function of optical depth, viz.,

相似文献    925. Results of TV imaging of Phobos (Experiment VSK-Fregat)      Avanesov G  Zhukov B  Ziman YA  Kostenko V  Kuzmin A  Murav'ev V  Fedotov V  Bonev B  Mishev D  Petkov D  Krumov A  Simeonov S  Boycheva V  Uzunov YU  Weide GG  Halmann D  Pössel W  Head J  Murchie S  Schkuratov YuG  Berghänel R  Danz M  Mangoldt T  Pihan U  Smith B 《Planetary and Space Science》1991,39(1-2):281-295 From February to March 1989 the Phobos 2 spacecraft took 37 TV images of Phobos at a distance of 190-1100 km. These images complement Mariner-9 and Viking data by providing higher-resolution coverage of a large region West of the crater Stickney (40-160 degrees W) and by providing disk-resolved measurements of surface brightness at a greater range of wavelengths and additional phase angles. These images have supported updated mapping and characterization of large craters and grooves, and have provided additional observations of craters' and grooves' bright rims. Variations in surface visible/near-infrared color ratio of almost a factor of 2 have been recognized; these variations appear to be associated with the ejecta of specific large impact craters. Updated determinations of satellite mass and volume allow calculation of a more accurate value of bulk density, 1.90 +/- 0.1 g cm-3. This is significantly lower than the density of meteoritic analogs to Phobos' surface, suggesting a porous interior perhaps containing interstitial ice.  相似文献    926. Shear-induced instability and arch filament eruption: A magnetohydrodynamic (MHD) numerical simulation      S. T. Wu  M. T. Song  P. C. H. Martens  M. Dryer 《Solar physics》1991,134(2):353-377 We investigate, via a two-dimensional (nonplanar) MHD simulation, a situation wherein a bipolar magnetic field embedded in a stratified solar atmosphere (i.e., arch-filament-like structure) undergoes symmetrical shear motion at the footpoints. It was found that the vertical plasma flow velocities grow exponentially leading to a new type of global MHD-instability that could be characterized as a Dynamic Shearing Instability, with a growth rate of about 8{ovV} A a, where {ovV} A is the average Alfvén speed and a –1 is the characteristic length scale. The growth rate grows almost linearly until it reaches the same order of magnitude as the Alfvén speed. Then a nonlinear MHD instability occurs beyond this point. This simulation indicates the following physical consequences: the central loops are pinched by opposing Lorentz forces, and the outer closed loops stretch upward with the vertically-rising mass flow. This instability may apply to arch filament eruptions (AFE) and coronal mass ejections (CMEs).To illustrate the nonlinear dynamical shearing instability, a numerical example is given for three different values of the plasma beta that span several orders of magnitude. The numerical results were analyzed using a linearized asymptotic approach in which an analytical approximate solution for velocity growth is presented. Finally, this theoretical model is applied to describe the arch filament eruption as well as CMEs.  相似文献    927. The Paasivaara PGE reef in the Penikat layered intrusion,northern Finland   总被引：1，自引：0，他引：1   Dr. T. A. Huhtelin  Prof. T. T. Alapieti  Dr. J. J. Lahtinen 《Mineralogy and Petrology》1990,42(1-4):57-70 Summary Three major PGE-bearing mineralized zones have been found in the layered series of the early Proterozoic Penikat layered intrusion. These are designated as the Sompujärvi (SJ), Ala-Penikka (AP) and Paasivaara (PV) Reefs according to the site of their initial discovery.The uppermost of these, the PV Reef, has the highest Pt/Pd ratio. It is located in the transition zone between the fourth and the fifth megacyclic units. The main host rock is the uppermost anorthosite, disseminated sulphides and associated PGM being concentrated in the interstices of this plagioclase orthocumulate. The Reef has also been encountered in other parts of the transition zone, however, and sometimes even in the lowermost parts of the fifth megacyclic unit. The dominant sulphide paragenesis is chalcopyrite-pyrrhotite-pentlandite, whereas the PGM identified are represented by sperrylite (PtAs2), kotulskite (PdTe), merenskyite (PdTe2), isomertieite (Pd11Sb2As2), stibiopalladinite (Pd5Sb2), cooperite (PtS) and braggite ((Pt, Pd, Ni)S).It is suggested that the PV Reef was formed in the mixing process when the fifth magma pulse intruded into the magma chamber. Mixing of the new magma with the older residual magma in the chamber accounted for the sulphide precipitation. Mixing and convection were probably turbulent at first and the sulphides were thus able to "scavenge" PGE from a large amount of silicate melt. The metal ratios in the mineralization point to a close genetic relationship with the fifth magma pulse. Das Paasivaara PGE Reef in der Penikat-Intrusion, Nord-Finnland Zusammenfassung In den geschichteten Serien der frühproterozoischen Intrusion von Penikat kommen drei grössere PGE-führende Zonen vor. Diese werden als die Sompujärvi (SJ), Ala-Penikka (AP) und Paasivaara (PV) Reefs bezeichnet, entsprechend den Lokalitäten der Entdeckung.Das am höchsten gelegene PV Reef hat die höchsten Pt/Pd Verhältnisse. Es liegt in der Übergangszone zwischen der vierten und der fünften megazyklischen Einheit. Das wichtigste Wirtsgestein ist der oberste Anorthosit, wo disseminierte Sulfide und assoziierte PGM in den Zwischenräumen dieses Plagioklas-Orthokumulates vorkommen. Das Reef wurde auch in anderen Teilen der Überganszone beobachtet und manchmal sogar in den untersten Partien der fünften megazyklischen Einheit. Die dominierende Sulfidparagenese ist Kupferkies-Magnetkies-Pentlandit; PGM sind Sperrylith (PtAs2), Kotulskit (PdTe), Merenskyit (PdTe2), Isomertieit (Pd11Sb2As2), Stibiopalladinit (Pd5Sb2), Cooperite (PtS) und Braggit ((Pt, Pd, Ni)S).Es wird angeregt, dass das PV Reef während der Mischungsvorgänge bei der Intrusion des fünften Magma Pulses in die Magmenkammer entstanden ist. Mischung des neuen Magmas mit dem alten Residual-Magma in der Kammer war für die Ausfällung der Sulfide verantwortlich. Mischung und Konvektion dürften anfangs turbulent gewesen sein, und so konnten die Sulfide die PGE aus einem beträchtlichen Anteil der Silikatschmelze entfernen. Die Metallverhältnisse dieser Vererzung lassen eine enge genetische Verbindung mit dem fünften Magmapuls erkennen. With 8 Figures  相似文献    928. Les gisements d'émeraude de la Cordillère Orientale de la Colombie: Nouvelles données métallogéniques      G. Giuliani  C. T. Rodriguez  F. Rueda 《Mineralium Deposita》1990,25(2):105-111 Emerald deposits of Colombia are confined to lower Cretaceous shales of the Eastern Cordillera. The tectonic pattern of the deposits is related to deep reverse and large regional fault systems. Hydrofracturing is the main factor controlling emerald mineralization. It permitted to the hydrothermal solutions to permeate through fractures but also along stratification planes forming in this case stratabound mineralizations. Emerald occurs in calcite veins, veinlets, pockets and brecciated zones associated mainly with pyrite, quartz, parisite, codazzite and fluorite. Emerald mineralization belongs to an epigenetic hydrothermal process. The alternance of arenite-shale formations in the Cretaceous probably played an important role in the accumulation of solutions and in the propagation of the hydrothermal channels. The origin of emerald involves chemical elements mobilized by the fluids in the Cr-V-Fe-Al-Si-bearing black shales. The source of beryllium remains a problem and is discussed in the paper.  相似文献    929. The structure of the broad line region in Fairall 9      Paul T. O'Brien  Wei Zheng 《Astrophysics and Space Science》1990,171(1-2):77-80 We find that the profile changes observed for the UV emission lines L,Civ 1549, and MgIII 2798, in the Seyfert 1 galaxy Fairall 9 occur mainly near the line centre for L andCiv and in the wings for MgIII. These results indicate that the broad line region (BLR) has a complex structure, possibly with non-spherical components.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.  相似文献    930. An optical transform and Monte Carlo study of the diffuse X-ray scattering in mullite,Al2(Al2+2xSi2−2x)O10−x      T. R. Welberry  R. L. Withers 《Physics and Chemistry of Minerals》1990,17(2):117-124 Diffuse X-ray scattering distributions have been recorded for reciprocal layers normal to c * of a synthetic mullite with composition Al2(Al2+2xSi2–2x) O10–xx, where represents an oxygen vacancy and x is close to 0.4. The effect on the diffuse scattering pattern of different schemes for ordering of the oxygen vacancies and the accompanying cation shifts within a single ab-layer of mullite has been investigated using optical diffraction analogue experiments in conjunction with Monte Carlo simulation.A simple scheme in which the only driving force for the ordering is that the Oc oxygens are precluded from being bonded to four T/T* cations, results in a 2D diffuse intensity distribution which displays many of the features that are observed in the x-ray scattering patterns. An alternative scheme in which bonding to four T/T* cations was favoured, resulted in a domain structure consisting of islands of the -alumina structure within a matrix of sillimanite. This gave diffraction patterns bearing no resemblance to the observed x-ray patterns and can, we believe, be discounted completely.  相似文献    [首页] « 上一页 [88] [89] [90] [91] [92] 93 [94] [95] [96] [97] [98] 下一页 » 末  页»