Synchrotron IR study of hydrous ringwoodite (γ-Mg2SiO4) up to 30 GPa

High-pressure synchrotron infrared (IR) absorption spectra were collected between 650 and 4,000 cm⁻¹ at ambient temperature for hydrous Mg-ringwoodite (γ-Mg₂SiO₄) up to 30 GPa. The main feature in the OH⁻ stretching region is an extremely broad band centred at 3,150 cm⁻¹. The hydrogen bond is strong for most protons and the most probable site for protonation is the tetrahedral edge. With increasing pressure, this band shifts downward while decreasing its integrated intensity until disappearance at a pressure of 25 GPa. Only one band at 2,450 cm⁻¹ and an absorption plateau persist with a maximum wavenumber of 3,800 cm⁻¹. This behaviour is reversible upon pressure release. We interpret this as a second-order phase transition occurring in hydrated Mg-ringwoodite at high pressure (beyond ∼ 25 GPa). This result is compatible with the observation by Kleppe et al. (Phys Chem Miner 29:473–476, 2002a) who suggested the presence of Si–O–Si linkages and/or partial increase in the coordination of Si. Beyond the phase transition, the protons are delocalized and their environment on the ringwoodite structure is probably quite different from that at low pressure. Data obtained in situ at high pressures and temperatures are needed to better understand the effect of protonation on the structure and to better constrain this phase transition.     

Large-scale phenomena on the Sun associated with the eruption of filaments outside active regions: the event of September 12, 1999

The event of September 12, 1999 is used to analyze large-scale disturbances associated with coronal mass ejections during the eruption of filaments outside active regions. The analysis is based on Hα filtergrams, EUV and soft X-ray images, and coronograph data. The filament eruption occurred in relatively weak magnetic fields, but was accompanied by larger-scale phenomena than flare events. During several hours after the eruption, a large-scale arcade developed, whose bases formed diverging flare-like ribbons. The volume of the event was bounded by an “EIT wave”, which was quasi-stationary at the solar surface and expanded above the limb. The event did not have an impulsive component; therefore the “EIT wave” above the limb was a magnetic structure, identified as the front of a coronal mass ejection by virtue of its shape, structural features, and kinematics. Three types of dimmings were observed within the areal of the event, cause by (a) the evacuation of plasma, (b) heating of plasma with its subsequent evacuation, and (c) the absorption of radiation in a system of filaments activated by the eruption. The fact that a dimming appeared due to plasma heating was revealed by its presence in soft X-rays, whereas the four EIT channels did not demonstrate this. This brings into question the correctness of certain conclusions drawn earlier based purely on EIT data. A transformation of magnetic fields brought about by the eruption also occurred in a stationary coronal hole adjacent to the areal of the event. The expansion of the coronal mass ejection was self-similar and characterized by a rapidly decreasing acceleration, which is not taken into account in the widely used polynomial approximation.     

The depositional environment of Mauddud limestone,Greater Burgan oil field,Kuwait

Six microfacies are defined on quantitative petrographic data in a carbonate/clastic sequence from the subsurface, oil producing Mauddud Formation of early Middle Cretaceous age. These are, in descending order of importance and abundance: (1) biomicritic wackestone-packstone, (2) argillaceous mudstone, (3) micritic mudstone, (4) glauconitic sandstone, (5)Orhitolina pelsparitic grainstone, and (6) argillaceous dolomite.Sedimentation took place during a marine transgression onto a very shallow, intertidal, restricted marine shelf lagoons. Facies variations appear to be related to depth and energy changes and proximity to areas of clastic deposition. These changes may have been controlled by slight tectonic events in the hinterland and changes in the rate of basin subsidence.

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Zusammenfassung Auf der Grundlage quantitativer petrographischer Daten werden sechs Mikrofazies in einer karbonat/klastischen Folge aus der unter der ErdoberflÄche liegenden, ölliefernden Mauddud-Formation der frühen Mittelkreide definiert. In absteigender Reihenfolge der Bedeutung und HÄufigkeit sind dieses: (1) biomikritischer wackestone-packstone, (2) toniger Schlickstein, (3) unkritischer Schlickstein, (4) glaukonitischer Sandstein, (5) Orbitolina-führender pelsparitischer Grainstone und (6) toniger Dolomit.Die Sedimentation erfolgte wÄhrend einer marinen Transgression auf sehr flache, intertidale Lagunen eines begrenzten marinen Schelfs. Die Fazies-Variationen scheinen mit den Wechseln in Wassertiefe und Energie sowie der mit NÄhe von Gebieten mit klastischer Sedimentation zusammenzuhÄngen.Diese Wechsel könnten durch kleinere tektonische Ereignisse im Hinterland und durch VerÄnderungen der Absenkungsrate des Beckens ausgelöst worden sein.

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Résumé Des données pétrographiques quantitatives permettent de définir six microfacies dans une série clasto-carbonatée d'âge crétacé inférieur du sous-sol de la région pé trolifère de Mauddud. Ce sont par ordre décroissant d'importance et d'abondance: (1) des wacstones-pacstone biomicritiques; (2) des argilites; (3) des argilites micritiques; (4) des grès glauconitiques; (5) des grainstone pelsparitiques à orbitolines; (6) des dolomies argileuses.La sédimentation se produisit au cours d'une transgression marine dans des lagunes très plates, intercotidales, d'une plate-forme continentale de faible étendue. Les variations de facies semblent Être dues à des changements de profondeur et d'énergie, ainsi qu'à la proximité de régions à sédimentation clastique.Ces changements pourraient résulter de légers mouvements tectoniques dans l'arrière-pays et de variations dans le degré de subsidence du bassin de sédimentation.

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- Mauddud, ( ). : 1) ; 2) ; 3) ; 4) ; 5) , 6) . , . , , , . , .

     

Vendian and Permian–Triassic Plagiogranite Magmatism of the Ust-Belaya Mountains,West Koryak Fold System,Northeastern Russia

Geotectonics - Vendian and Permian–Triassic plagiogranite magmatism is distinguished for the Ust-Belsky and Algansky terranes of West Koryak fold system. The U‒Pb zircon ages from...     

Magnetic anomalies of offshore Krishna-Godavari basin,eastern continental margin of India

The marine magnetic data acquired from offshore Krishna-Godavari (K-G) basin, eastern continental margin of India (ECMI), brought out a prominent NE-SW trending feature, which could be explained by a buried structural high formed by volcanic activity. The magnetic anomaly feature is also associated with a distinct negative gravity anomaly similar to the one associated with 85°E Ridge. The gravity low could be attributed to a flexure at the Moho boundary, which could in turn be filled with the volcanic material. Inversion of the magnetic and gravity anomalies was also carried out to establish the similarity of anomalies of the two geological features (structural high on the margin and the 85°E Ridge) and their interpretations. In both cases, the magnetic anomalies were caused dominantly by the magnetization contrast between the volcanic material and the surrounding oceanic crust, whereas the low gravity anomalies are by the flexures of the order of 3–4 km at Moho boundary beneath them. The analysis suggests that both structural high present in offshore Krishna-Godavari basin and the 85°E Ridge have been emplaced on relatively older oceanic crust by a common volcanic process, but at discrete times, and that several of the gravity lows in the Bay of Bengal can be attributed to flexures on the Moho, each created due to the load of volcanic material.     

The Bikkulovskoe manganese deposit (South Urals): Geological setting,composition of metalliferous rocks,and formation model

The results of investigation of the Bikkulovskoe manganese deposit confined to volcanosedimentary piles of the Magnitogorsk paleovolcanic belt are presented. The paper characterizes the geological setting of the deposit and mineral-chemical compositions of ores and enclosing rocks (volcanomictic sandstones; ferruginous, manganiferous, and ferruginous-siliceous tuffites; and jasperites). Analysis of the data obtained made it possible to identify four sequential stages of deposit formation: (1) accumulation and diagenesis of ore-bearing sequences (D_2–3); (2) burial and low-grade (T = 200–250°C, P = 2 to 3 kbar) regional metamorphism of rocks (D_2–3-C₁); (3) tectonic deformations of volcanosedimentary piles (C₂-P); and (4) hypergenesis and partial denudation of rocks (MZ-CZ). According to the model proposed for the accumulation of ore-bearing rocks, the productive member was formed in a zone of hydrothermal solution outflow to the seafloor surface. Discharge of solutions and precipitation of Fe and Si began below the seafloor surface (rather than above the surface) in the near-bottom sequence of volcanomictic sediments. Upon reaching the seafloor, the impoverished solutions mixed with seawater and gave up metals completely: Fe and Mn were transferred to sediments to make up the ore-bearing bed. Thus, zonal sediments with ferruginous tuffites at the base and manganese ores at the top were formed.     

Melting of albite and dehydration of brucite in H2O–NaCl fluids to 9 kbars and 700–900°C: implications for partial melting and water activities during high pressure metamorphism

 The melting reaction: albite_(solid)+ H₂O_(fluid) =albite-H₂O_(melt) has been determined in the presence of H₂O–NaCl fluids at 5 and 9.2 kbar, and results compared with those obtained in presence of H₂O–CO₂ fluids. To a good approximation, albite melts congruently at 9 kbar, indicating that the melting temperature at constant pressure is principally determined by water activity. At 5 kbar, the temperature (T)- mole fraction (X _(H2O) ) melting relations in the two systems are almost coincident. By contrast, H₂O–NaCl mixing at 9 kbar is quite non-ideal; albite melts ∼70 ^°C higher in H₂O–NaCl brines than in H₂O–CO₂ fluids for X _(H2O) =0.8 and ∼100 ^°C higher for X _(H2O) =0.5. The melting temperature of albite in H₂O–NaCl fluids of X _(H2O)=0.8 is ∼100 ^°C higher than in pure water. The P–T curves for albite melting at constant H₂O–NaCl show a temperature minimum at about 5 kbar. Water activities in H₂O–NaCl fluids calculated from these results, from new experimental data on the dehydration of brucite in presence of H₂O–NaCl fluid at 9 kbar, and from previously published experimental data, indicate a large decrease with increasing fluid pressure at pressures up to 10 kbar. Aqueous brines with dissolved chloride salt contents comparable to those of real crustal fluids provide a mechanism for reducing water activities, buffering and limiting crustal melting, and generating anhydrous mineral assemblages during deep crustal metamorphism in the granulite facies and in subduction-related metamorphism. Low water activity in high pressure-temperature metamorphic mineral assemblages is not necessarily a criterion of fluid absence or melting, but may be due to the presence of low a _(H2O) brines. Received: 17 March 1995/Accepted: 9 April 1996     

The flux deficits in star spots

The bolometric flux deficits of the photospheres of spotted stars are derived for the first time in the framework of zonal spottedness models for red dwarfs computed at the Crimean Astrophysical Observatory. The resulting flux deficits are compared to the estimated radiative losses from the chromospheres and coronas measured during quasi-simultaneous observations. A linear correlation is found between the logarithms of these quantities, with the Sun fitting these relations. Radiative losses from the outer stellar atmospheres in quiescence and during individual sporadic flares are significantly lower than the bolometric deficits of the spotted photospheres of active stars. This suggests that the flux deficit due to spots leads to global reconstruction of the atmospheres of red dwarfs, analogous to the local atmospheric reconstruction that occurs during solar and stellar flares. This process may be realized via the superposition of a large number of weak impulsive flares and other dynamic events, which develop on these stars and heat their coronas (i.e., in this view, microflaring is favored as the principal coronal heating mechanism for these stars). A brief analysis of the long-term variations in the chromospheric and photospheric radiation of F-K stars from the HK project and of the Sun suggests that such dynamical reconstruction of the outer atmosphere by energy associated with the flux deficit of the spotted photosphere occurs at times of increased surface activity in all F-M stars.     

TEM soundings in magnetic media

TEM responses of conducting ferromagnetic materials to a complex current pulse have been modeled for a magnetic cylinder typical of well casing. The behavior of the responses is investigated as a function of different model parameters.