Simulation of liquefaction beneath an impermeable surface layer     

N. Yoshida  W. D. L. Finn   《Soil Dynamics and Earthquake Engineering》2000,19(5)

A joint element is proposed, which can simulate the three phases of behaviour of an impermeable layer over a liquefied sand layer. The analysis tracks the post-liquefaction reconsolidation of the sand, the simultaneous development of a water film between the layers and the settlements resulting from the subsequent drainage of the water film. The element is incorporated in a finite element program, which can be used to simulate the behaviour of layered systems. The effectiveness of the program is demonstrated by simulation of the performance of a model soil deposit of two layers in a centrifuge test.  相似文献   

Ion upflow and downflow at the topside ionosphere observed by the EISCAT VHF radar   总被引：2，自引：0，他引：2  

M. Endo  R. Fujii  Y. Ogawa  S. C. Buchert  S. Nozawa  S. Watanabe  N. Yoshida 《Annales Geophysicae》2000,18(2):170-181

We have determined the MLT distribution and KpK_P dependence of the ion upflow and downflow of the thermal bulk oxygen ion population based on a data analysis using the EISCAT VHF radar CP-7 data obtained at Tromsø during the period between 1990 and 1996: (1) both ion upflow and downflow events can be observed at any local time (MLT), irrespective of dayside and nightside, and under any magnetic disturbance level, irrespective of quiet and disturbed levels; (2) these upflow and downflow events are more frequently observed in the nightside than in the dayside; (3) the upflow events are more frequently observed than the downflow events at any local time except midnight and at any K_P level and the difference of the occurrence frequencies between the upflow and downflow events is smaller around midnight; and (4) the occurrence frequencies of both the ion upflow and downflow events appear to increase with increasing KP level, while the occurrence frequency of the downflow appears to stop increasing at some KP level  相似文献   

Triassic to Early Jurassic (c. 200 Ma) UHP metamorphism in the Central Rhodopes: evidence from U–Pb–Th dating of monazite in diamond‐bearing gneiss from Chepelare (Bulgaria)          下载免费PDF全文

I. Petrík  M. Janák  N. Froitzheim  N. Georgiev  K. Yoshida  V. Sasinková  P. Konečný  S. Milovská 《Journal of Metamorphic Geology》2016,34(3):265-291

Evidence for ultrahigh‐pressure metamorphism (UHPM) in the Rhodope metamorphic complex comes from occurrence of diamond in pelitic gneisses, variably overprinted by granulite facies metamorphism, known from several areas of the Rhodopes. However, tectonic setting and timing of UHPM are not interpreted unanimously. Linking age to a metamorphic stage is a prerequisite for reconstruction of these processes. Here, we use monazite in diamond‐bearing gneiss from Chepelare (Bulgaria) to date the diamond‐forming UHPM event in the Central Rhodopes. The diamond‐bearing gneiss comes from a strongly deformed, lithologically heterogeneous zone (Chepelare Mélange) sandwiched between two migmatized orthogneiss units, known as Arda‐I and Arda‐II. Diamond, identified by Raman micro‐spectroscopy, shows the characteristic band mostly centred between 1332 and 1330 cm^?1. The microdiamond occurs as single grains or polyphase diamond + carbonate inclusions, rarely with CO₂. Thermodynamic modelling shows that garnet was stable at UHP conditions of 3.5–4.6 GPa and 700–800 °C, in the stability field of diamond, and was re‐equilibrated at granulite facies/partial melting conditions of 0.8–1.2 GPa and 750–800 °C. The texture of monazite shows older central parts and extensive younger domains which formed due to metasomatic replacement in solid residue and/or overgrowth in melt domains. The monazite core compositions, with distinctly lower Y, Th and U contents, suggest its formation in equilibrium with garnet. The U–Th–Pb dating of monazite using electron microprobe analysis yielded a c. 200 Ma age for the older cores with low Th, Y, U and high La/Nd ratio, and a c. 160 Ma age for the dominant younger monazite enriched in Th, Y, U and HREE. The older age of c. 200 Ma is interpreted as the timing of UHPM, whereas the younger age of c. 160 Ma as granulite facies/partial melting overprint. Our results suggest that UHPM occurred in Late Triassic to Early Jurassic time, in the framework of collision and subduction of continental crust after the closure of Paleotethys.  相似文献   

Statistical distribution of gravitational-lensing excursion angles: winding ways to us from the deep Universe     

Takashi Hamana  Matthias Bartelmann  Naoki Yoshida  Christoph Pfrommer 《Monthly notices of the Royal Astronomical Society》2005,356(3):829-838

We investigate statistical distributions of differences in gravitational-lensing deflections between two light rays, the so-called lensing excursion angles. A probability distribution function of the lensing excursion angles, which plays a key role in estimates of lensing effects on angular clustering of objects (such as galaxies, quasi-stellar objects and also the cosmic microwave background temperature map), is known to consist of two components: a Gaussian core and an exponential tail. We use numerical gravitational-lensing experiments in a ΛCDM cosmology for quantifying these two components. We especially focus on the physical processes responsible for generating these two components. We develop a simple empirical model for the exponential tail which allows us to explore its origin. We find that the tail is generated by the coherent lensing scatter by massive haloes with   M > 10¹⁴  h ⁻¹ M_⊙  at   z < 1  and that its exponential shape arises due to the exponential cut-off of the halo mass function at that mass range. On scales larger than 1 arcmin, the tail does not have a practical influence on the lensing effects on the angular clustering. Our model predicts that the coherent scatter may have non-negligible effects on angular clustering at subarcminute scales.  相似文献   

Modelling peculiar velocities of dark matter haloes     

Takashi Hamana  Issha Kayo  Naoki Yoshida  Yasushi Suto  Y. P. Jing 《Monthly notices of the Royal Astronomical Society》2003,343(4):1312-1318

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Quasi-radial modes of rotating stars in general relativity     

Shin'ichirou Yoshida  Yoshiharu Eriguchi 《Monthly notices of the Royal Astronomical Society》2001,322(2):389-396

By using the Cowling approximation, quasi-radial modes of rotating general relativistic stars are computed along equilibrium sequences from non-rotating to maximally rotating models. The eigenfrequencies of these modes are decreasing functions of the rotational frequency. The eigenfrequency curve of each mode as a function of the rotational frequency has discontinuities, which arise from the avoided crossing with other curves of axisymmetric modes.  相似文献   

Oscillations of vertically integrated relativistic tori – I. Axisymmetric modes in a Schwarzschild space–time     

Luciano Rezzolla  Shin'ichirou Yoshida  Olindo Zanotti 《Monthly notices of the Royal Astronomical Society》2003,344(3):978-992

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Can non-Gaussian cosmological models explain the WMAP high optical depth for reionization?     

Xuelei Chen  Asantha Cooray  Naoki Yoshida  Naoshi Sugiyama 《Monthly notices of the Royal Astronomical Society》2003,346(3):L31-L35

The first-year Wilkinson Microwave Anisotropy Probe data suggest a high optical depth for Thomson scattering of  0.17 ± 0.04  , implying that the Universe was reionized at an earlier epoch than previously expected. Such early reionization is likely to be caused by ultraviolet (UV) photons from first stars, but it appears that the observed high optical depth can be reconciled within the standard structure formation model only if star formation in the early Universe was extremely efficient. With normal star formation efficiencies, cosmological models with non-Gaussian density fluctuations may circumvent this conflict as high density peaks collapse at an earlier epoch than in models with Gaussian fluctuations. We study cosmic reionization in non-Gaussian models and explore to what extent, within available constraints, non-Gaussianities affect the reionization history. For mild non-Gaussian fluctuations at redshifts of 30 to 50, the increase in optical depth remains at a level of a few per cent and appears unlikely to aid significantly in explaining the measured high optical depth. On the other hand, within available observational constraints, increasing the non-Gaussian nature of density fluctuations can easily reproduce the optical depth and may remain viable in underlying models of non-Gaussianity with a scale-dependence.  相似文献   

High accretion rate during class 0 phase due to external trigger     

Kazutaka Motoyama  Tatsuo Yoshida 《Monthly notices of the Royal Astronomical Society》2003,344(2):461-467

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Finite source effect on the polarization degree induced by a single microlens     

Hiroshi Yoshida 《Monthly notices of the Royal Astronomical Society》2006,369(2):997-1008

We investigate the effect of a single microlens on Stokes parameters. Semi-analytical formulae of the microlensed Stokes parameters are derived. The formulae not only reduce the double integrals in the estimations of those quantities but can also be approximated to a useful form in the bypass case. By using our formulation, we show that a combination of polarimetric data with photometric data enables us to estimate not only the finite source effect but also the direction of the microlens motion.  相似文献