Time-series of δ26Mg values in a headwater catchment reveal decreasing magnesium isotope variability from precipitation to runoff

Data on temporal variability in Mg isotope ratios of atmospheric deposition and runoff are critical for decreasing the uncertainty associated with construction of isotope mass balances in headwater catchments, and statistical evaluation of isotope differences among Mg pools and fluxes. Such evaluations, in turn, are needed to distinguish between biotic and abiotic contributions to Mg²⁺ in catchment runoff. We report the first annual time-series of δ²⁶Mg values simultaneously determined for rainfall, canopy throughfall, soil water and runoff. The studied 55-ha catchment, situated in western Czech Republic, is underlain by Mg-rich amphibolite and covered by mature spruce stands. Between 1970 and 1996, the site received extremely high amounts of acid deposition and fly ash form nearby coal-burning power plants. The δ²⁶Mg values of open-area precipitation (median of −0.79‰) at our study site were statistically indistinguishable from the δ²⁶Mg values of throughfall (−0.73‰), but significantly different from the δ²⁶Mg values of soil water (−0.55‰) and runoff (−0.55‰). The range of δ²⁶Mg values during the observation period decreased in the order: open-area precipitation (0.57‰) > throughfall (0.27‰) > runoff (0.21‰) > soil water (0.16‰). The decreasing variability in δ²⁶Mg values of Mg²⁺ from precipitation to soil water and runoff reflected an increasing homogenization of atmospheric Mg in the catchment and its mixing with geogenic Mg. In addition to atmospheric Mg, runoff also contained Mg mobilized from the three major solid Mg pools, bedrock (δ²⁶Mg of −0.32‰), soil (−0.28‰), and vegetation (−0.31‰). The drought of summer 2019 did not affect the nearly constant δ²⁶Mg value of runoff. Collectively, our data show that within-catchment processes buffer the Mg isotope variability of the atmospheric input.     

Agricolaite, a new mineral of uranium from J��chymov, Czech Republic

The new mineral agricolaite, a potassium uranyl carbonate with ideal formula K₄(UO₂)(CO₃)₃, occurs in vugs of ankerite gangue in gneisses in the abandoned Giftkiesstollen adit at Jáchymov, Czech Republic. The name is after Georgius Agricola (1494?C1555), German scholar and scientist. Agricolaite occurs as isolated equant irregular translucent grains to 0.3?mm with yellow color, pale yellow streak, and vitreous luster. It is brittle with uneven fracture and displays neither cleavage nor parting. Agricolaite is non-fluorescent. Mohs hardness is ~4. It is associated with aragonite, brochantite, posnjakite, malachite, rutherfordine, and ??pseudo-voglite??. Experimental density is higher than 3.3?g.cm^?3, Dcalc is 3.531?g.?cm^?3. The mineral is monoclinic, space group C2/c, with a 10.2380(2), b 9.1930(2), c 12.2110(3) ?, ?? 95.108(2)°, V 1144.71(4) ?³, Z?=?4. The strongest lines in the powder X-ray diffraction pattern are d(I)(hkl): 6.061(55)(002), 5.087(57)(200), 3.740(100)(202), 3.393(43)(113), 2.281(52)(402). Average composition based on ten electron microprobe analyses corresponds to (in wt.%) UO₃ 48.53, K₂O 31.49, CO₂(calc) 22.04 which gives the empirical formula K_3.98(UO₂)_1.01(CO₃)_3.00. The crystal structure was solved from single-crystal X-ray diffraction data and refined to R ₁?=?0.0184 on the basis of the 1,308 unique reflections with F _o?>?4??F _o. The structure of agricolaite is identical to that of synthetic K₄(UO₂)(CO₃)₃ and consists of separate UO₂(CO₃)₃ groups organized into layers parallel to (100) and two crystallographically non-equivalent sites occupied by K⁺ cations. Both the mineral and its name were approved by the IMA-CNMNC.     

Is Phobos Magnetized?

The available experimental data and theoretical reasons allow us to point out only the upper limit of Phobos' magnetic moment, which does not exceed 10¹⁸ G cm³.     

Comparative analysis of recurrent high-speed solar wind streams influence on the radiation environment of near-earth space in April–July 20101

This paper analyzes variations of flux of relativistic and subrelativistic electrons in the outer radiation belt of the Earth caused by the arrival of recurrent high-speed streams of solar wind during three consecutive solar rotations. The period from April to July 2010 is covered. During this time, an increase in fluxes of relativistic electrons was observed after they had reached a minimum in November 2009–January 2010. Two coronal holes of different polarity, geometry, and location relative to the solar equator were the source of high-speed solar wind streams. The relationship between the efficiency of acceleration of electrons of subrelativistic energies and the amplitude, duration of high-speed streams of solar wind and geomagnetic disturbances, as well as the wave activity in the range of 2–7 mHz, characterized by the ULF index, is confirmed. Significant increases of the flux of relativistic electrons in the outer radiation belt of the Earth were observed during the considered period with an hourly average speed of solar wind streams above 550 km/s and a duration of more than seven days. It is found that the spectrum of electrons in the Earth’s outer radiation belt over the considered period of time was softer during the observation of solar wind streams from the positive polarity coronal hole, even given the amplitude of the solar wind velocity higher than 550 km/s.     

Statistics of isolated and complex geomagnetic storms based on the APEV database for cycle 23 of solar activity

The development of geomagnetic storms is mainly controlled by external heliospheric factors, which in turn depend on the conditions on the Sun. Magnetospheric disturbances can be isolated, repeated, multiple, or turbulent, depending on these conditions. Most geomagnetic storms develop complexly and are characterized by the existence of one or several side extrema before or after the main one. This is mainly related to the superposition of individual disturbances that follow immediately one after another from the Sun into the heliosphere or to the internal structure and dynamics of disturbances in the corona. The geomagnetic storms from the APEV extensive database for cycle 23 of solar activity, which were combined into 227 events, were analyzed in order to reveal the statistics based on single and multiple magnetospheric disturbances. The results are presented as histograms, graphs, tables, and empirical formulas for the total number of intensifications in all events and depending on different geomagnetic storm development phases, amplitude, and duration.     

Optimization of the interplanetary energetic proton flux database and its application in modeling radiation conditions

The dissimilarity of the results of solar and galactic proton flux measurements made on different spacecraft is pointed out. It is caused, in addition to instrument errors, by differences in the temporal and spatial conditions of the measurements. We suggest using statistical analysis of proton fluences calculated for different long time intervals, from half a year to 10 years, for the optimization of the interplanetary proton database. An example of such analysis is presented and a probabilistic model of total proton fluences at the Earth’s orbit outside the magnetosphere, constructed using the analysis, is described. A formalized method for separating proton fluxes in solar proton events from protons of galactic cosmic rays is suggested. A conclusion is made that sources of cosmic ray protons with energies of less than 4 MeV should be examined in more detail.     

Mineralogy of PGE in the mafic-ultramafic massifs of the Kola region

Summary During the last few years nearly 50 minerals and unnamed platinum-group element (PGE) phases have been identified by the authors in nickel-bearing mafic-ultramafic massifs of the Kola region. About 20 established PGE minerals have been found whilst more than 20 previously undescribed and unnamed PGE phases can be reported. In addition high concentrations of these elements in sulfarsenides of the cobaltitegersdorffite series have been established. The PGE phases form tiny (5–70 µm, seldom larger) mono- and polymineral inclusions in the main sulfides of the nickel-copper mineralization; at the contacts with silicates and within the silicates themselves. The details of the composition of platinum mineralization in various massifs, its formation under magmatic and hydrothermal conditions and wide isomorphism in certain groups of minerals have been established. Specific features of PGE mineralization of the region as a whole are: the predominance of bismuth tellurides and arsenides of palladium and platinum, a highly subordinated role of their sulphides and higher concentrations of several PGE in sulfarsenides.

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Platingruppen-Minerale in den mafischen-ultramafischen Intrusionen der Kola Region

Zusammenfassung In den vergangenen Jahren wurden etwa 50 z.T. noch unbekannte Minerale von Platingruppen-Elementen (PGE) in Ni-führenden mafisch-ultramafischen Gesteinen der Kola Region bestimmt (ca. 20 bereits bakannte und mehr also 20 bisher nicht beschriebene bzw. noch unbenannte PGE-Minerale). Außerdem wurden hohe Konzentrationen dieser Elemente in Sulfarseniden der Cobaltit-Gersdorffit-Reihe nachgewiesen.Die PGE-Minerale kommen als mono- und polymineralische Einschlüsse in den Sulfiden der Ni-Cu-Mineralisation, am Kontakt der Sulfide zu den Silikaten und in den Silikaten selbst vor. Details über die PGE-Mineralisation in verschiedenen Gebieten, ihre Bildung unter magmatischen und hydrothermalen Bedingungen und die Isomorphiebeziehungen innerhalb bestimmter Mineralgruppen werden dargestellt.Spezifische Eigenheiten der PGE-Mineralisation dieser Region sind: Das Vorherrschen von wismutvtelluriden, sowie von Pd- und Pt-Arseniden, die untergeordnete Rolle von Pd- und Pt-Sulfiden und erhöhte Gehalte bestimmter PGE in den Sulfarseniden.

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Contribution to the Fifth International Platinum Symposium, Helsinki, August 1989.

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With 2 Figures     

Paleomagnetism of the Siberian traps: New data and a new overall 250 Ma pole for Siberia

The flood basalt province in Siberia is one of the largest in the world but the number of reliable paleomagnetic data on these volcanics is still limited. We studied lava flows and trap-related intrusions from two areas in the north and west of the Siberian platform. A dual-polarity characteristic component was isolated from most samples with the aid of stepwise thermal and alternating field demagnetization. We then compiled all published paleomagnetic data on the Siberian traps that have been obtained according to modern standards; also included are presumably trap-related overprint directions in Paleozoic rocks. Although these overprints and trap results may locally differ, the corresponding mean poles based on remagnetized sediments and volcanics show excellent overall agreement and justify pooling of both data types. Several ways of data grouping were attempted; the trap mean pole proved to be rather insensitive to statistical treatment. Irrespective of the averaging procedure used, the overall mean poles for the Siberian traps (NSP2: 55.1°N, 147.0°E; N = 8, K = 123, A₉₅ = 5.0° or NSP4: 57.2°N, 151.1°E; N = 8, K = 192, A₉₅ = 4.0°) differ slightly, but significantly from the coeval mean poles of Baltica [Torsvik, 2001; Van der Voo, R., and Torsvik, T.H., The quality of the European Permo-Triassic paleopoles and its impact on Pangea reconstructions, in: Timescales of the Paleomagnetic Field, J. E. T. Channell, D.V. Kent, W. Lowrie, and J.G. Meert, eds., AGU Geophys. Monogr., 2004, 135, 29–42]. We consider possible causes for this difference and conclude that it could be explained either by persistent non-dipole terms in the Permo-Triassic geomagnetic field or widespread inclination shallowing in the European data.     

Studying correlations between the coronal hole area,solar wind velocity,and local magnetic indices in the Canadian region during the decline phase of cycle 23

Geomagnetic disturbances in the Canadian region are compared with their solar and heliospheric sources during the decline phase of solar activity, when recurrent solar wind streams from low-latitude coronal holes were clearly defined. A linear correlation analysis has been performed using the following data: the daily and hourly indices of geomagnetic activity, solar wind velocity, and coronal hole area. The obtained correlation coefficients were rather low between the coronal hole areas and geomagnetic activity (0.17–0.48), intermediate between the coronal hole areas and the solar wind velocity (0.40–0.65), and rather high between the solar wind velocity and geomagnetic activity (0.50–0.70). It has been indicated that the correlation coefficient values can be considerably increased (by tens of percent in the first case and about twice in the second case) if variations in the studied parameters related to changes in the ionosphere (different illumination during a year) and variations in the heliolatitudinal shift of the coordinate system between the Earth, the Sun, and a spacecraft are more accurately taken into account.