The crystal structure of sarkinite,Mn2AsO4(OH)

Summary Sarkinite is a basic manganese arsenate, Mn₂AsO₄(OH). The lattice parameters are:a=12.779 (2) Å,b=13.596 (2) Å,c=10.208 (2) Å, =108°53 (6). Space groupP2₁/a,Z=16. The crystal structure has been solved by direct methods from three-dimensional X-ray diffractometer data and refined by least-squares methods toR=0.052 for 3519 independent reflections. The crystal structure is built up by a three-dimensional framework of MnO₄(OH)₂ octahedra, MnO₄(OH) trigonal bipyramids and AsO₄ tetrahedra, as found in wagnerite. Isotypy of sarkinite with triploidite is confirmed.

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Die Kristallstruktur des Sarkinits, Mn₂AsO₄(OH)

Zusammenfassung Die Kristallstruktur des basischen Manganarsenates Sarkinit, Mn₂AsO₄(OH), mit den Gitterkonstantena=12,779 (2) Å,b=13,596 (2) Å,c=10,208 (2) Å, =108°53 (6). RaumgruppeP2₁/a,Z=16, wurde mit dreidimensionalen Röntgendiffraktometermessungen durch direkte Methoden gelöst und nach dem kleinste-Quadrate-Verfahren verfeinert (R=0,052 für 3519 unabhängige Reflexe). Die Struktur besteht aus einem dreidimensionalen Gerüst aus MnO₄(OH)₂-Oktaedern, trigonalen Bipyramiden von MnO₄(OH) und AsO₄-Tetraedern wie in Wagnerit. Die Isotypie von Sarkinit mit Triploidit wurde bestätigt.

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Selection criteria for linear regression models to estimate individual tree biomasses in the Atlantic Rain Forest,Brazil

Background

Biomass models are useful for several purposes, especially for quantifying carbon stocks and dynamics in forests. Selecting appropriate equations from a fitted model is a process which can involves several criteria, some widely used and others used to a lesser extent. This study analyzes six selection criteria for models fitted to six sets of individual biomass collected from woody indigenous species of the Tropical Atlantic Rain Forest in Brazil. Six models were examined and the respective fitted equations evaluated by the residual sum of squares, adjusted coefficient of determination, absolute and relative estimates of the standard error of estimate, and Akaike and Schwartz (Bayesian) information criteria. The aim of this study was to analyze the numeric behavior of these model selection criteria and discuss the ease of interpretation of them. The importance of residual analysis in model selection is stressed.

Results

The adjusted coefficient of determination (\( R^{2}_{adj.} \)) and the standard error of estimate in percentage (Syx%) are relative model selection criteria and are not affected by sample size and scale of the response variable. The sum of squared residuals (SSR), the absolute standard error of estimate (Syx), the Akaike information criterion and the Schwartz information criterion, in turn, depend on these quantities. The best fit model was always the same within a given data set regardless the model selection criteria considered (except for SSR in two cases), indicating they tend to converge to a common result. However, such criteria are not always closely related across different data sets. General model selection criteria are indicative of the average goodness of fit, but do not capture bias and outlier effects. Graphical residual analysis is a useful tool to this detection and must always be used in model selection.

Conclusions

It is concluded that the criteria for model selection tend to lead to a common result, regardless their mathematical formulation and statistical significance. Relative measures of goodness of fitting are easier to interpret than the absolute ones. Careful graphical residual analysis must always be used to confirm the performance of the models.

     

Non-diffusive propagation of ultra high energy cosmic rays

We report the results of 3D simulations of non-diffusive propagation of Ultra High Energy Cosmic Rays (UHECR) (E > 10²⁰ eV) through the intergalactic and extended halo media. We quantify the expected angular and temporal correlations between the events and the sources, and the temporal delay between protons and gamma-ray counterparts with a common origin for both halo and extragalactic origins. It is shown that the proposed UHECR-supergalactic plane source associations require either extremely high values of the halo magnetic field over as much as 100 kpc length scale or a very large correlation length for the IGM, even for the largest possible values of the intergalactic magnetic field. It can be stated that the UHECR seem to point to the sources even more strongly than previously believed. The simulations also show that the calculated time delays between UHE protons and gamma-ray counterparts do not match the claimed GRB-UHECR associations for either cosmological or extended halo distance scales.     

How Cr<Superscript>3+</Superscript> and Fe<Superscript>3+</Superscript> affect Mg–Al order–disorder transformation at high temperature in natural spinels

Three natural Mg(Al_2-yCr_y)O₄ spinels (y 0.07–0.16), highly ordered in terms of Mg–Al, and one Mg(Al_2–yFe³⁺_y)O₄ spinel (y0.08), highly ordered also in terms of Fe³⁺, were studied by means of X-ray single-crystal diffraction. All samples were heated in situ from 25 to 1000 °C in order to follow both thermal expansion and evolution of the structural state of spinel with temperature. Thermal expansion was monitored by means of the variation of cell edge a with temperature, and found to be well represented throughout the temperature range by a regression line a = a₀ (1+T), slightly different at lower and higher temperatures. Thermal expansion coefficient ₁, referring to the lower temperature range (i.e. during pure thermal expansion), was slightly lower than ₂, calculated only over the highest temperatures. The trend showed different slopes for individual crystals. Structural evolution with temperature was studied by means of the variation of oxygen positional parameter u, which is strongly influenced by intersite cation exchange and thus closely correlated with inversion parameter x. In particular, in the three Cr samples, in which Cr resides only in the octahedral site, u parameter variations and hence the order–disorder process, started at about 700 °C. Instead, in the Fe³⁺ sample, this process was triggered at lower temperatures, starting at 550 °C with Fe³⁺–Mg exchange followed at higher temperatures by that of Mg–Al. Cr contents in the Cr samples affected the occupancy of Al in the tetrahedral site at the highest temperatures. In both Mg–Al–Cr and Mg–Al–Fe³⁺ compositions, if CrFe³⁺, parameter u reached the same value only when the Mg–Al exchange was dominant, i.e. at the highest temperatures, but not before. Cation distribution at each temperature was obtained by the bond-length model, applying thermal expansion to pure bond lengths. This method is applied here to complex compositions for the first time.     

Availability and use of willow species in representative cold desert areas of northwestern himalaya, India

Willow species(Salix fragilis L.and S.alba L.) are important elements of cold desert agroforestry systems in the Lahaul valley,northwestern Himalaya.Their ability to grow through shoot-cuttings plantations under extreme and xeric climatic conditions of cold deserts,makes them ecologically suited and socially accepted for forestry programmes.Willow species in cold deserts may combat desertification and can thrive well in these areas as compared to any other species.Salix fragilis L.and S.alba L.are under cultivation in the Lahaul valley.However,S.fragilis is widely cultivated under the agroforestry and plantation forestry systems.In the Lahaul valley,willow species are used as subsistence resources and for socio-religious purposes.The present study was carried out to examine the vegetation analysis,density,diversity and distribution of willow species,present status and potential willow plantation sites and uses.The results of present study revealed that a higher species density was recorded at middle altitude villages(Jahlma-3,000 m asl and Hinsa-2,700 m asl),except,a higher density of S.fragilis was at Khoksar(3,200 m asl) in plantation forestry on south-facing slopes.In forests,S.fragilis was planted mainly along the water channels,resulted a low density.The shrubby willow species occurred naturally in the entire Lahaul valley up to an altitude of 3,850 m asl.81% of households felt the scarcity of willow trees,whereas,19% of households were satisfied with the willow trees they owned.The majority of willow species were planted in middle altitudes on privately owned irrigated lands.It was rated most potential prospective willow planting site by the farmers.Small size of land-holdings was one of the main constraints for establishing a large number of willow plantations.Commercial aspects of willow species need to be investigated to encourage the farmers to plant more willows further.     

The dynamics of velocity fluctuations in the solar wind – I. Coronal mass ejections

In this paper we present a simple, analytic model for the dynamical evolution of supersonic velocity fluctuations at the base of the ambient solar wind. These fluctuations result in the formation of dense working surfaces that travel down the wind. It is shown how the initial parameters of the fluctuations (velocity, density and duration) are related to the characteristics of the working surfaces far from the Sun (for instance at the Earth). We apply the model to the evolution of the coronal mass ejections in the IP medium, finding that the model is in good agreement with satellite observations of these phenomena, thus providing physical insight into their dynamical evolution. Our model may contribute to future 'space weather forecasting' on the Earth, based on detailed satellite monitoring of the solar corona.     

Comparison Between Halo cme Expansion Speeds Observed on the Sun,the Related Shock Transit Speeds to Earth and Corresponding Ejecta Speeds at 1 au

We have compared characteristics of 38 halo coronal mass ejections observed on the Sun by the Large Angle and Spectrometric Coronagraph onboard SOHO with their corresponding counterparts observed near Earth by the magnetic field and plasma instruments onboard the ACE, WIND and SOHO satellites, in the period from January 1997 to April 2001. We only have selected events that have some associated interplanetary ejecta structure at 1 AU and we have compared the lateral expansion speeds of these halo CMEs and the corresponding ejecta speeds near Earth. We found that there is a high correlation between these two speeds. The results are very similar to the study done by Lindsay et al. (1999) using observations made by Solwind and SMM coronagraphs, and Helios-1 and PVO plasma and interplanetary field data from the period of 1979 to 1988. Also, we reviewed the relation between the CME-related shock transit speed to Earth and the ejecta speeds near Earth. This kind of relation is very important to estimate ejecta speeds of events for which no interplanetary observations are available.