Identification in the Ca II K spectral region of sharp-lined B- type stars

Previous Call K observations of the B-type star HD 83206 have revealed putative high-velocity interstellar clouds (HVCs) at Local Standard of Rest (LSR) velocities of -80 and -110 km s(- 1). Similar results were also found for the sightline towards HD135485. In this article, we show that these absorption lines are in fact due tr, stellar SII features. As the Call K absorption line in B-type stars is often used to assess the presence and distance of HVCs. we also present a very high quality spectrum of HD 83206 in the Ca II K region (similar to+/-4 Angstrom or +/-300 km s(-1)), so that in the future confusion between stellar lines and HVC features may be avoided.

Ca II K observations of QSOs in the line-of-sight to the Magellanic Bridge

We describe medium-resolution spectroscopic observations taken with the ESO Multi-Mode Instrument (EMMI) in the CaII K line (lambda air = 3933.661 angstrom) towards 7 QSOs located in the line-of-sight to the Magellanic Bridge. At a spectral resolution R =lambda/Delta lambda = 6000, five of the sightlines have a signal-to-noise ( S/N) ratio of similar to 20 or higher. Definite Ca absorption due to Bridge material is detected towards 3 objects, with probable detection towards two other sightlines. Gas-phase CaII K Bridge and Milky Way abundances or lower limits for the all sightlines are estimated by the use of Parkes 21-cm H. emission line data. These data only have a spatial resolution of 14 arcmin compared with the optical observations which have milli-arcsecond resolution. With this caveat, for the three objects with sound CaII K detections, we find that the ionic abundance of CaII K relative to HI, A = log( N( CaK)/ N( HI)) for low- velocity Galactic gas ranges from - 8.3 to - 8.8 dex, with HI column densities varying from 3- 6 x 10(20) cm(-2). For Magellanic Bridge gas, the values of A are similar to 0.5 dex higher, ranging from similar to- 7.8 to - 8.2 dex, with N( HI) = 1- 5 x 1020 cm(-2). Higher values of A correspond to lower values of N( HI), although numbers are small. For the sightline towards B 0251 - 675, the Bridge gas has two different velocities, and in only one of these is CaII tentatively detected, perhaps indicating gas of a different origin or present-day characteristics ( such as dust content), although this conclusion is uncertain and there is the possibility that one of the components could be related to the Magellanic Stream. Higher signal-to-noise CaII K data and higher resolution H. data are required to determine whether A changes with N( HI) over the Bridge and if the implied difference in the metalicity of the two Bridge components towards B 0251-675 is real.

Inorganic synthesis of Fe-Ca-Mg carbonates at low temperature

A set of free-drift experiments was undertaken to synthesize carbonates of mixed cation content (Fe, Ca, Mg) from solution at 25 and 70 degrees C to better understand the relationship between the mineralogy and composition of these phases and the solutions from which they precipitate. Metastable solid solutions formed at 25 degrees C which are not predicted from the extrapolation of higher temperature equilibrium assemblages; instead, solids formed that were intermediary in chemical composition to known magnesite-siderite and dolomite solid solutions. A calcite-siderite solid solution precipitated at 25 degrees C, with the percentage of CaCO3 in the solid being proportional to the aqueous Ca/Fe ratio of the solution, while Mg was excluded from the crystal structure except at relatively high aqueous Mg/Ca and Mg/Fe ratios and a low Ca content. Alternatively, at 70 degrees C Mg was the predominant cation of the solid solutions. These results are compatible with the hypothesis that the relative dehydration energies of Fe, Ca and Mg play an important role in the formation of mixed cation carbonates in nature. (C) 2009 Elsevier Ltd. All rights reserved.

Análise de crescimento em Heteranthera reniformis, sob diferentes teores de Ca, Mg e S

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Variabilidade espacial do pH, Ca, Mg e V% do solo em diferentes formas do relevo sob cultivo de cana-de-açúcar

Em uma paisagem natural, os solos apresentam uma ampla variação dos atributos químicos, tanto vertical como horizontal, resultante da interação dos diversos fatores de formação envolvidos. Este trabalho foi desenvolvido em Guariba-SP, com o objetivo de avaliar a variabilidade espacial do pH, cálcio (Ca), magnésio (Mg) e saturação por bases (V%) em um Latossolo Vermelho eutroférrico sob cultivo de cana-de-açúcar, utilizando-se métodos da estatística clássica, análise geoestatística e técnica de interpolação de dados, com a finalidade de observar padrões de ocorrência destes atributos na paisagem. No terço inferior da encosta, após análise detalhada da variação do gradiente do declive, caracterizaram-se dois compartimentos (I e II), sob os quais os solos foram amostrados nos pontos de cruzamento de uma malha, com intervalos regulares de 50m, perfazendo um total de 206 pontos, nas profundidades de 0,0-0,2m e 0,6-0,8m. Os maiores alcances foram observados na profundidade de 0,0-0,2m para todos os atributos estudados, com exceção do cálcio que apresentou comportamento inverso, refletindo os efeitos do maior grau de intemperismo e do manejo na variabilidade natural dos solos. Pequenas variações, nas formas do relevo, condicionam variabilidade diferenciada para os atributos químicos.

Determination of Ca, Mg, and Zn in biodiesel microemulsions by FAAS using discrete nebulization

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Acúmulo de nutrientes e relação Ca:Mg no cultivo da cebola, no submédio São Francisco

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Determinação direta de Ca, Mg, Mn e Zn em amostras de leite de búfala da Ilha de Marajó por espectrometria de absorção atômica com chama (FAAS)

ABSTRACT: This work proposes an analytical procedure for direct determination of calcium, magnesium, manganese and zinc in buffalo milk by flame atomic absorption spectrometry (FAAS). Samples were diluted with a solution containing 10% (v/v) of water-soluble tertiary amines (CFA-C) at pH 8. For comparison, buffalo milk samples were digested with HNO₃ and H₂O₂. According to a paired t-test, the results obtained in the determination of Ca, Mg, Mn and Zn in digested samples and in 10% (v/v) CFA-C medium were in agreement at a 95% confidence level. The developed procedure is simple, rapid, decrease the possibility of contamination and can be applied for the routine determination of Ca, Mg, Mn and Zn in buffalo milk samples without any difficulty caused by matrix constituents, such as fat content, and particle size distribution in the milk emulsion

Functional Mn-Mg-k cation complexes in GaN featured by Raman spectroscopy

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Extraktion und nanoanalytische Charakterisierung refraktärer Nanometallpartikel frühester solarer Materie und Synthese metallischer Nanopartikel aus dotierten Ca-Mg-Al-Si-Schmelzen

Primitive kohlige Chondrite sind Meteorite, die seit ihrer Entstehung im frühen Sonnensystem kaum verändert wurden und dadurch einen Einblick in Prozesse geben, die zur Bildung und Veränderung der ersten festen Materie führten. Solche Prozesse können anhand von Bruchstücken dieser Meteorite detailliert im Labor studiert werden, sodass Rückschlüsse auf die Entwicklung unseres Sonnensystems im frühen Stadium getroffen werden können. Ca-, Al-reiche Einschlüsse (CAIs) aus chondritischen Meteoriten sind die ersten Festkörper des Sonnensystems und enthalten viele refraktäre Metallnuggets (RMNs), welche hauptsächlich aus den Elementen Os, Ir, Ru, Mo und Pt bestehen. Nach weit verbreiteter Ansicht sind diese Nuggets wahrscheinlich im Gleichgewicht mit dem solaren Nebel kondensiert, bereits früher oder gleichzeitig mit Oxiden und Silikaten. Die exakten Mechanismen, die zu ihren heute beobachteten Eigenschaften führten, sind allerdings unklar. Um frühere Arbeiten fortzuführen, wurde eine hohe Anzahl RMNs in vier unterschiedlichen Typen von Meteoriten detailliert studiert, darunter solche aus dem nahezu unveränderten Acfer 094, Allende (CV3ox), Leoville (CV3red) und Murchison (CM2). Die RMNs wurden in-situ, assoziiert mit ihren Wirtsmineralen und auch in Säurerückständen gefunden, deren Präparationsprozedur in dieser Arbeit speziell für RMNs durch eine zusätzliche Dichtetrennung verbessert wurde.rnDie Ergebnisse decken eine Reihe von Ungereimtheiten zwischen den beobachteten RMN-Eigenschaften und einer Kondensationsherkunft auf, sowohl für Kondensation in solarer Umgebung, als auch für Kondensation aus Material von Supernovae oder roten Riesen, für die die Kondensationssequenzen refraktärer Metalle speziell für diesen Vergleich berechnet wurden. Stattdessen wurden in dieser Arbeit neue Einblicke in die RMN-Entstehung und die Entwicklung der ersten Festkörper (CAIs) durch eine Kombination aus experimentellen, isotopischen, strukturellen und petrologischen Studien an RMNs gewonnen. Viele der beobachteten Eigenschaften sind mit Ausfällung der RMN aus einer CAI-Schmelze vereinbar. Ein solches Szenario wird durch entsprechende Untersuchungen an synthetisch hergestellten, mit refraktären Metallen im Gleichgewicht stehenden CAI-Schmelzen bestätigt. Es folgt aus den Ergebnissen, dass die Mehrzahl der RMNs isotopisch solar ist und alle untersuchten RMNs innerhalb von CAIs bei rascher Abkühlung (um bis zu 1000 °C/40 sek.) einer CAI-Schmelze gebildet wurden. rn