Функціональні особливості антропонімів англійської мови (на матеріалі англійської художньої літератури) (The functional pecuilarities of anthroponyms of the English language (on the material of English fiction literature))

У статті розглянуто проблему функціональності антропонімів англійської мови. Автором відзначено вплив соціальних та культурних аспектів на антропонімічну систему англійської мови. Англійські антропоніми не є виключенням в цьому аспекті, але водночас, вони зумовлюються семантичними та фонетичними особливостями англійської мови. У художньому тексті вони можуть виконувати різноманітні функції, автором наведено приклади антропонімів, які виконують функції алюзії, порівняння, метафори та катафоричну функції.Дослідницею визначено, що антропоніми несуть в собі соціальний та національний компоненти. Вони, також, виконують функції позначення особистої культурної ідентичності людини та водночас виконують об’єднувальну функцію у питанні між- культурної комунікації. (The aricle deals with the problem of functioning of anthroponyms in the English language. The author has pointed the influence of social and cultural aspects on the anthroponym system of the English language. English anthroponyms are conditioned by semantic and phonetic features of the language. In the fiction text they may have different functions, the author has given the examples of allusion, comparison, metaphor and cataphoric functions that have anthroponyms. The researcher has determined that anthroponyms include social and national components. They have also the function of determining of person’s cultural identity and at the same time they have the connectional function in the question of intercultural communication.

Primitive Terrestrial Xenon: A Relation to Refined Composition of Solar Wind

To explain the isotopic structure of terrestrial Xe, a hypothetical U-Xe (unrelated to uranium) was mathematically constructed using multidimensional correlation diagrams of stepwise heating data of carbonaceous chondrites [1]. The composition of U-Xe was derived without any references to solar Xe. Nevertheless U-Xe turned out to be almost identical to Solar Wind (SW) except for two heaviest isotopes ^(136)Xe and ^(134)Xe, in which U-Xe was depleted. The mismatch in these two heaviest Xe isotopes was attributed to either the presence of nearly pure Xe-H (heavy branch of Xe-HL) in the Sun or to deficit of Xe-H in the carbonaceous chondrites from which U-Xe composition has been de-rived. There are two difficulties in this approach: U-Xe has never been reproducibly observed and Xe-H and Xe-L are apparently inseparable

Heavy noble gases in solar wind delivered by Genesis mission

One of the major goals of the Genesis Mission was to refine our knowledge of the isotopic composition of the heavy noble gases in solar wind and, by inference, the Sun, which represents the initial composition of the solar system. This has now been achieved with permil precision: ^(36)Ar/^(38)Ar = 5.5005 ± 0.0040, ^(86)Kr/^(84)Kr = .3012 ± .0004, ^(83)Kr/^(84)Kr = .2034 ± .0002, ^(82)Kr/^(84)Kr = .2054 ± .0002, ^(80)Kr/^(84)Kr = .0412 ± .0002, ^(78)Kr/^(84)Kr = .00642 ± .00005, ^(136)Xe/^(132)Xe = .3001 ± .0006, ^(134)Xe/^(132)Xe = .3691 ± .0007, ^(131)Xe/^(132)Xe = .8256 ± .0012, ^(130)Xe/^(132)Xe = .1650 ± .0004, ^(129)Xe/^(132)Xe = 1.0405 ± .0010, ^(128)Xe/^(132)Xe = .0842 ± .0003, ^(126)Xe/^(132)Xe = .00416 ± .00009, and ^(124)Xe/^(132)Xe = .00491 ± .00007 (error-weighted averages of all published data). The Kr and Xe ratios measured in the Genesis solar wind collectors generally agree with the less precise values obtained from lunar soils and breccias, which have accumulated solar wind over hundreds of millions of years, suggesting little if any temporal variability of the isotopic composition of solar wind krypton and xenon. The higher precision for the initial composition of the heavy noble gases in the solar system allows (1) to confirm that, exept ^(136)Xe and ^(134)Xe, the mathematically derived U–Xe is equivalent to Solar Wind Xe and (2) to provide an opportunity for better understanding the relationship between the starting composition and Xe-Q (and Q-Kr), the dominant current “planetary” component, and its host, the mysterious phase-Q

Evidence of presolar SiC in the Allende Curious Marie calcium–aluminium-rich inclusion

Calcium–aluminium-rich inclusions (CAIs) are one of the first solids to have condensed in the solar nebula, while presolar grains formed in various evolved stellar environments. It is generally accepted that CAIs formed close to the Sun at temperatures above 1,500 K, where presolar grains could not survive, and were then transported to other regions of the nebula where the accretion of planetesimals took place. In this context, a commonly held view is that presolar grains are found solely in the fine-grained rims surrounding chondrules and in the low-temperature fine-grained matrix that binds the various meteoritic components together. Here we demonstrate, on the basis of noble gas isotopic signatures, that presolar SiC grains were incorporated into fine-grained CAIs in the Allende carbonaceous chondrite at the time of their formation, and have survived parent-body processing. This finding provides new clues on the conditions in the nascent Solar System at the condensation of the first solids

I-Xe studies of aqueous alteration in the Allende CAI Curious Marie

The Allende fine-grained inclusion Curious Marie is a unique CAI. It is depleted in uranium but contains large ^(235)U excess [1], providing new evidence that ^(247)Cm was alive in the Early Solar System, as has been previously suggested [2], and leading to an updated (^(247)Cm/^(235)U)initial ratio of (1.1±0.3)×10^(-4)

Weak decay of 130 Ba and 132 Ba : Geochemical measurements

The half-life of 130Ba due to multichannel weak decay (2β+, 2EC, and ECβ+) has been determined for the first time by the measurement of the 130Xe daughter accumulated in natural barite (BaSO4) from the Belorechenskoe deposit in North Caucasus, Russia. The accumulation time was determined from U-Xe and K-Ar gas-retention ages measured in the same material, yielding a half-life for 130Ba for all weak decay modes of 2.2±0.5×1021yr (68% C.L.), about a factor of 2 lower than that predicted by the proton-neutron quasiparticle random phase approximation. From excess 132Xe observed in this barite, the half-life for weak decay of 132Ba can be estimated (T1/2=1.3±0.9×1021yr). However, this value is more tentative, since other sources of this isotope cannot be excluded, but the lower limit of 2.2×1021yr remains firm

I-Xe studies of aqueous alteration in the Allende CAI Curious Marie

The Allende fine-grained inclusion Curious Marie is a unique CAI. It is depleted in uranium but contains large ^(235)U excess [1], providing new evidence that ^(247)Cm was alive in the Early Solar System, as has been previously suggested [2], and leading to an updated (^(247)Cm/^(235)U)initial ratio of (1.1±0.3)×10^(-4)