排序方式： 共有21条查询结果，搜索用时 31 毫秒
1.
We study in some detail one-dimensional NLTE effects in solar Fei lines. The lines selected are frequently used in solar polarimetry, and also in studies of line asymmetries and for abundance determinations. Our model atom for Fei–Feii–Feiii is realistic: it takes account of multiplet structure and it includes over 200 bound–bound and bound–free transitions in detail. We use very efficient iterative methods for the self-consistent solution of the kinetic and radiative transfer equations (Auer, Fabiani Bendicho, and Trujillo Bueno, 1994). We have applied these fast methods of solution because they are suitable for the investigation of 2D and 3D NLTE transfer effects with multilevel atoms, which constitutes the next step of our ongoing research project on the iron line formation problem. 相似文献
2.
Shchukina Elena V. Agashev Aleksey M. Soloshenko Natalia G. Streletskaya Mariya V. Zedgenizov Dmitry A. 《Mineralogy and Petrology》2019,113(5):593-612
Mineralogy and Petrology - In this paper, new main and trace elements and isotopic data are presented for 14 coarse-grained eclogite xenoliths from the V. Grib kimberlite pipe in the central part... 相似文献
3.
4.
A. V. Zubkova N. I. Kobanov A. A. Sklyar R. I. Kostyk N. G. Shchukina 《Astronomy Letters》2014,40(4):222-229
We analyze the oscillations of the Hα profile width based on our observations of the chromosphere at the base of solar coronal holes. The maximum oscillation amplitude averaged over ten time series is 64 m 0 A. Direct calculations show that this value cannot be reached through temperature oscillations, because the periodic intensity fluctuations observed during our experiment did not exceed 5%, corresponding to Hα profile broadening only by 1.5–2 m Å. We hypothesize that the observed variations can result from the propagation of torsional Alfvén waves in the chromosphere of coronal holes. 相似文献
5.
6.
E. V. Shchukina N. N. Golovin V. G. Mal’kovets N. P. Pokhilenko 《Doklady Earth Sciences》2012,444(2):776-781
This study presents mineralogical and thermobarometric data for equilibrium peridotite assemblages from the V. Grib kimberlite pipe of the Arkhangelsk diamond province. We provided the first constraints on the composition, structure, thermal state, and lower boundary of the lithospheric mantle beneath the V. Grib kimberlite pipe. It was found that phlogopite-free and phlogopite-bearing peridotite xenoliths can be distinguished by their mineral chemistry. The occurrence of phlogopite in peridotites may represent evidence for modal metasomatism responsible for variation in the mineral composition of phlogopite-pyrope and pyrope peridotites. On the basis of P-T estimates, we conclude that modal metasomatism may have affected the entire thickness of the lithospheric mantle beneath the V. Grib kimberlite pipe. Comparison of our results with the available data from the literature shows strong vertical and lateral mantle heterogeneity beneath kimberlite pipes of the Lomonosov deposit and the V. Grib pipe. 相似文献
7.
V. L. Ol’shevskii N. G. Shchukina I. E. Vasil’eva 《Kinematics and Physics of Celestial Bodies》2008,24(3):145-158
We consider the NLTE formation of the resonance Ba II line λ 455.4 nm in the solar spectrum for three one-dimensional and one three-dimensional hydrodynamic models of the quiet solar atmosphere. The sensitivity of the line to atomic parameters, microturbulent and macroturbulent velocities, as well as to oscillator strength and barium abundance uncertainties was examined. The wings of the barium line are shown to be most sensitive to the van der Waals broadening constant. Another important parameter is the barium abundance. Our NLTE estimate of the solar barium abundance (A Ba = 2.16) derived with allowance made for the nonuniform solar atmosphere structure is in good agreement with earlier results. The influence of granular convective motions on the line profile shape was studied, and the profiles formed in granules and in intergranular lanes are shown to be asymmetric and differently shaped. We demonstrate that the theoretical profiles match well the observed ones when the NLTE effects and the granular structure are taken into account. 相似文献
8.
This paper presents new major and trace element data from 150 garnet xenocrysts from the V. Grib kimberlite pipe located in the central part of the Arkhangelsk diamondiferous province (ADP). Based on the concentrations of Cr2O3, CaO, TiO2 and rare earth elements (REE) the garnets were divided into seven groups: (1) lherzolitic “depleted” garnets (“Lz 1”), (2) lherzolitic garnets with normal REE patterns (“Lz 2”), (3) lherzolitic garnets with weakly sinusoidal REE patterns (“Lz 3”), (4) lherzolitic garnets with strongly sinusoidal REE patterns (“Lz 4”), (5) harzburgitic garnets with sinusoidal REE patterns (“Hz”), (6) wehrlitic garnets with weakly sinusoidal REE patterns (“W”), (7) garnets of megacryst paragenesis with normal REE patterns (“Meg”). Detailed mineralogical and geochemical garnet studies and modeling results suggest several stages of mantle metasomatism influenced by carbonatite and silicate melts. Carbonatitic metasomatism at the first stage resulted in refertilization of the lithospheric mantle, which is evidenced by a nearly vertical CaO-Cr2O3 trend from harzburgitic (“Hz”) to lherzolitic (“Lz 4”) garnet composition. Harzburgitic garnets (“Hz”) have probably been formed by interactions between carbonatite melts and exsolved garnets in high-degree melt extraction residues. At the second stage of metasomatism, garnets with weakly sinusoidal REE patterns (“Lz 3”, “W”) were affected by a silicate melt possessing a REE composition similar to that of ADP alkaline mica-poor picrites. At the last stage, the garnets interacted with basaltic melts, which resulted in the decrease CaO-Cr2O3 trend of “Lz 2” garnet composition. Cr-poor garnets of megacryst paragenesis (“Meg”) could crystallize directly from the silicate melt which has a REE composition close to that of ADP alkaline mica-poor picrites. P-T estimates of the garnet xenocrysts indicate that the interval of ～60–110 km of the lithospheric mantle beneath the V. Grib pipe was predominantly affected by the silicate melts, whereas the lithospheric mantle deeper than 150 km was influenced by the carbonatite melts. 相似文献
9.
10.
NLTE formation of the silicon spectrum is studied in three one-dimensional semiempirical models of the solar atmosphere: HOLMUL, MACKKL, and VAL,C. The NLTE silicon abundance calculated from 65 Si I lines of different strengths is almost independent of the excitation potentials, wavelengths, and equivalent widths if the van der Waals damping constant ??6 is calculated using the Unsold approximation with an enhancement factor E = 1.5. The NLTE silicon abundance range from 7.547 ± 0.012 (HOLMUL) to 7.582 ± 0.013 (VAL,C). The use of the Anstee-Barklem-O??Mara (ABO) theory to calculate ??6 leads to a decrease in the silicon abundance with an increase in the equivalent widths. It is found that the NLTE silicon abundance corrections are, on average, ?0.05 dex. The errors in the NTLE abundance due to uncertainties in the cross sections of photoionization and inelastic collisions with electrons and hydrogen atoms are 0.02 dex or less. It is shown that the use of the shifted Gurtovenko-Kostyk ??solar?? oscillator-strength scale instead of the experimental scale proposed by Becker et al. gives almost the same silicon abundance. 相似文献