Математическая психология

The article is devoted to mathematical psychology. The processes associated with the emergence of mathematical psychology and its stages. Definition of the problem of limited modeling capabilities with the help of this psychology. We consider in this article are still major areas of mathematical professor psychology V.Krylov (he played a leading role in the development of mathematical psychology)

“Dogged” Search of Fresh Nakhla Surfaces Reveals New Alteration Textures

Special Issue: 74th Annual Meeting of the Meteoritical Society, August 8-12, 2011, London, U.K.International audienceCarbonaceous chondrites are considered as amongst the most primitive Solar System samples available. One of their primitive characteristics is their enrichment in volatile elements.This includes hydrogen, which is present in hydrated and hydroxylated minerals. More precisely, the mineralogy is expected to be dominated by phyllosilicates in the case of CM chondrites, and by Montmorillonite type clays in the case of CI. Here, in order to characterize and quantify the abundance of lowtemperature minerals in carbonaceous chondrites, we performed thermogravimetric analysis of matrix fragments of Tagish Lake, Murchison and Orgueil

Coordinated Microanalyses of Seven Particles of Probable Interstellar Origin from the Stardust Mission

Stardust, a NASA Discovery-class mission, was the first sample-return mission to return solid samples from beyond the Moon. Stardust was effectively two missions in one spacecraft: it returned the first materials from a known primitive solar system body, the Jupiter-family comet Wild 2; Stardust also returned a collector that was exposed to the contemporary interstellar dust stream for 200 days during the interplanetary cruise. Both collections present severe technical challenges in sample preparation and in analysis. By far the largest collection is the cometary one: approximately 300 micro g of material was returned from Wild 2, mostly consisting of approx. 1 ng particles embedded in aerogel or captured as residues in craters on aluminum foils. Because of their relatively large size, identification of the impacts of cometary particles in the collection media is straightforward. Reliable techniques have been developed for the extraction of these particles from aerogel. Coordinated analyses are also relatively straightforward, often beginning with synchrotron-based x-ray fluorescence (S-XRF), X-ray Absorption Near-Edge Spectoscopy (XANES) and x-ray diffraction (S-XRD) analyses of particles while still embedded in small extracted wedges of aerogel called ``keystones'', followed by ultramicrotomy and TEM, Scanning Transmission X-ray Microscopy (STXM) and ion microprobe analyses (e.g., Ogliore et al., 2010). Impacts in foils can be readily analyzed by SEM-EDX, and TEM analysis after FIB liftout sample preparation. In contrast, the interstellar dust collection is vastly more challenging. The sample size is approximately six orders of magnitude smaller in total mass. The largest particles are only a few pg in mass, of which there may be only approx.10 in the entire collection. The technical challenges, however, are matched by the scientific importance of the collection. We formed a consortium carry out the Stardust Interstellar Preliminary Examination (ISPE) to carry out an assessment of this collection, partly in order to characterize the collection in sufficient detail so that future investigators could make well-informed sample requests. The ISPE is the sixth PE on extraterrestrial collections carried out with NASA support. Some of the basic questions that we asked were: how many impacts are there in the collector, and what fraction of them have characteristics consistent with extraterrestrial materials? What is the elemental composition of the rock-forming elements? Is there crystalline material? Are there organics? Here we present coordinated microanalyses of particles captured in aerogel, using S-FTIR, S-XRF, STXM, S-XRD; and coordinated microanalyses of residues in aluminum foil, using SEMEDX, Auger spectroscopy, STEM, and ion microprobe. We discuss a novel approach that we employed for identification of tracks in aerogel, and new sample preparation techniques developed during the ISPE. We have identified seven particles - three in aerogel and four in foils - that are most consistent with an interstellar origin. The seven particles exhibit a large diversity in elemental composition. Dynamical evidence, supported supported by laboratory simulations of interstellar dust impacts in aerogel and foils, and numerical modeling of interstellar dust propagation in the heliosphere, suggests that at least some of the particles have high optical cross-section, perhaps due to an aggregate structure. However, the observations are most consistent with a variety of morphologie

Final Reports of the Stardust ISPE: Seven Probable Interstellar Dust Particles

The Stardust spacecraft carried the first spaceborne collector specifically designed to capture and return a sample of contemporary interstellar dust to terrestrial laboratories for analysis [1]. The collector was exposed to the interstellar dust stream in two periods in 2000 and 2002 with a total exposure of approximately 1.8 10(exp 6) square meters sec. Approximately 85% of the collector consisted of aerogel, and the remainder consisted of Al foils. The Stardust Interstellar Preliminary Examination (ISPE) was a consortiumbased effort to characterize the collection in sufficient detail to enable future investigators to make informed sample requests. Among the questions to be answered were these: How many impacts are consistent in their characteristics with interstellar dust, with interplanetary dust, and with secondary ejecta from impacts on the spacecraft? Are the materials amorphous or crystalline? Are organics detectable? An additional goal of the ISPE was to develop or refine the techniques for preparation, analysis, and curation of these tiny samples, expected to be approximately 1 picogram or smaller, roughly three orders of magnitude smaller in mass than the samples in other small particle collections in NASA's collections - the cometary samples returned by Stardust, and the collection of Interplanetary Dust Particles collected in the stratosphere

Mineralogy and petrology of comet 81P/wild 2 nucleus samples

The bulk of the comet 81P/Wild 2 (hereafter Wild 2) samples returned to Earth by the Stardust spacecraft appear to be weakly constructed mixtures of nanometer-scale grains, with occasional much larger (over 1 micrometer) ferromagnesian silicates, Fe-Ni sulfides, Fe-Ni metal, and accessory phases. The very wide range of olivine and low-Ca pyroxene compositions in comet Wild 2 requires a wide range of formation conditions, probably reflecting very different formation locations in the protoplanetary disk. The restricted compositional ranges of Fe-Ni sulfides, the wide range for silicates, and the absence of hydrous phases indicate that comet Wild 2 experienced little or no aqueous alteration. Less abundant Wild 2 materials include a refractory particle, whose presence appears to require radial transport in the early protoplanetary disk

X‐Rays Analysis for Space Sciences: X‐Ray Fluorescence Spectroscopy

International audienceX-ray analysis was introduced at the beginning of the twentieth century, right after the discovery of X-rays. It represents a specific group of methods of investigation of samples that share the same probe, the X-rays, and produces nondestructive, highly varied results of the intrinsic properties of specimens. X-ray fluorescence (XRF) is the main method of X-ray analysis and, as such, constitutes the subject of this article, where it is applied to the priceless astromaterials, better known as extraterrestrial samples. These comprise recorded falls (meteorites), samples collected in space, and sample return mission (SRM) specimens brought back to Earth by space missions, or simply by in situ measurements on Solar System bodies, or from remote orbital or flyby analyses thereof

NanoXRF elemental mapping of Middle Jurassic (~-170Ma) coccoliths

International audienceCoccolithophores algae produce micrometric calcite platelets called coccoliths. Coccoliths geological record is continuous from their appearance 220 Ma ago until today and are found in abundant marine environment in this time interval. Hence, coccoliths have huge potential for geochemical reconstruction of paleoclimate and paleoceanography through time. We have performed nanometric XRF analysis on 3 species of Early Bajocian (Middle Jurassic) coccoliths at European Synchrotron Radiation Facility (ESRF) on the beamline ID22NI, Grenoble, France. Based on this analysis, we endeavor to have a better understanding of the chemical composition of coccoliths and thus of marine waters where they were precipitated. Samples have been collected at Cabo Mondego, Portugal, the international reference section (GSSP) for the Early Bajocian interval and they were selected based on their preservation. Beforehand, coccoliths were separated from the matrix using a picking technique and deposited on 500 nm-thick silicon nitride membranes. With an excitation beam at 17 KeV and a resolution of 100 m, we have mapped 14 elements in coccoliths, i.e., S, Cl, K, Ca, Ti, V, Cr, Mn, Fe, Cu, Zn, Br, Rb and Sr. The mapping allows the recognition of biological incorporation of elements from the diagenetic overprint. Calcium, Strontium and Manganese are biologically organized in coccoliths. Sulfur, Chlorine, Chromium, and Bromine are also homogenously incorporated without relation with the crystallographic organization of the coccolith. Conversely, Potassium, Iron, Copper, Zinc, Titanium and Rubidium are related to diagenetic processes and clays contamination. These results will (1) help in a better understanding of the chemical incorporation of elements, and (2) in the recognition of diagenetic effects on coccoliths chemistry, and finally (3) develop new paleoceanographic proxies, e.g. the Chlorine and Bromine incorporation in coccoliths for salinity reconstructions. Further analysis especially on living species will greatly help in the calibration of such a proxy