辽宁庄河地区构造变形及构造演化初探     

秦松贤  吕贻峰  李江风 《国土资源》1995,(2)

辽宁庄河地区构造活动强烈，构造变形样式多种多样，反映了在不同体制下，构造变形由下部构造层次到上部构造层次的系统变化，从早期褶皱变形到后则破裂变形过程中岩石韧性递减的系统演变。笔者利用构造解析方法，初步确定了该区的构造序列并探讨了构造演化过程。  相似文献   

阿尔金造山带东段地质构造演化概论     

郑健康 《青海国土经略》1995,(2)

阿尔金造山带曾是一个早古生代拗拉槽,其两侧地质体具有极为相似的地质构造特征。该区构造演化可以概括为:晚太古代至早元古代处于底侵造壳阶段,经吕梁旋回发生克拉通化,出现中元古代稳定型盖层沉积。加里东旋回中叶,经过短暂的拗拉、裂陷,分裂的塔柴板块又重新聚合。华力西旋回该区以剥蚀夷平作用为主,仅在山间断陷或山前凹陷的局部地段沉积有上泥盆统磨拉石建造。石炭纪发生短暂小规模海侵。侏罗纪全区进入陆相发育阶段。区内岩浆活动频繁,燕山旋回为最高潮。在喜山旋回,随着印度板块与欧亚板块的碰撞,该区也被卷入青藏高原总体的巨大演变之中。早期由边缘断陷转化为大型断陷盆地,至上新世湖水淹没了大部地区;晚期,随着阿尔金迅速崛起,塔里木—柴达木板块再度分裂,南盘抬升,北盘下降。文章最后探讨了阿尔金左行斜滑地震断裂带的控震作用。  相似文献   

Cosmological smoothed particle hydrodynamics simulations: the entropy equation   总被引：2，自引：0，他引：2  

Volker Springel  Lars Hernquist 《Monthly notices of the Royal Astronomical Society》2002,333(3):649-664

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A cosmological study of the star formation history in the solar neighbourhood     

X. Hernández  Vladimir Avila-Reese  Claudio Firmani 《Monthly notices of the Royal Astronomical Society》2001,327(1):329-338

We use a cosmological galactic evolutionary approach to model the Milky Way. A detailed treatment of the mass aggregation and dynamical history of the growing dark halo is included, together with a self-consistent physical treatment for the star formation processes within the growing galactic disc. This allows us to calculate the temporal evolution of star and gas surface densities at all galactic radii, in particular, the star formation history (SFH) at the solar radius. A large range of cosmological mass aggregation histories (MAHs) is capable of producing a galaxy with the present-day properties of the Milky Way. The resulting SFHs for the solar neighbourhood bracket the available observational data for this feature, the most probable MAH yielding the optimal comparison with these observations. We also find that the rotation curve for our Galaxy implies the presence of a constant density core in its dark-matter halo.  相似文献   

Saturn's cloud structure and temporal evolution from ten years of Hubble Space Telescope images (1994-2003)     

S. Pérez-Hoyos  A. Sánchez-Lavega  J.F. Rojas 《Icarus》2005,176(1):155-174

We present a study of the vertical structure of clouds and hazes in the upper atmosphere of Saturn's Southern Hemisphere during 1994-2003, about one third of a Saturn year, based on Hubble Space Telescope images. The photometrically calibrated WFPC2 images cover the spectral region between the near-UV (218-255 nm) and the near-IR (953-1042 nm), including the 890 nm methane band. Using a radiative transfer code, we have reproduced the observed center-to-limb variations in absolute reflectivity at selected latitudes which allowed us to characterize the vertical structure of the entire hemisphere during this period. A model atmosphere with two haze layers has been used to study the variation of hazes with latitude and to characterize their temporal changes. Both hazes are located above a thick cloud, putatively composed of ammonia ice. An upper thin haze in the stratosphere (between 1 and 10 mbar) is found to be persistent and formed by small particles (radii ∼0.2 μm). The lower thicker haze close to the tropopause level shows a strong latitudinal dependence in its optical thickness (typically τ∼20-40 at the equator but τ∼5 at the pole, at 814 nm). This tropospheric haze is blue-absorbent and extends from 50 to 100 mbar to about ∼400 mbar. Both hazes show temporal variability, but at different time-scales. First, there is a tendency for the optical thickness of the stratospheric haze to increase at all latitudes as insolation increases. Second, the tropospheric haze shows mid-term changes (over time scales from months to 1-2 years) in its optical thickness (typically by a factor of 2). Such changes always occur within a rather narrow latitude band (width ∼5-10°), affecting almost all latitudes but at different times. Third, we detected a long-term (∼10 year) decrease in the blue single-scattering albedo of the tropospheric haze particles, most intense in the equatorial and polar areas. Long-term changes follow seasonal insolation variations smoothly without any apparent delay, suggesting photochemical processes that affect the particles optical properties as well as their size. In contrast, mid-term changes are sudden and show various time-scales, pointing to a dynamical origin.  相似文献   

Semi-analytic simulations of galactic winds: volume filling factor, ejection of metals and parameter study     

Serena Bertone †  Felix Stoehr  Simon D. M. White 《Monthly notices of the Royal Astronomical Society》2005,359(4):1201-1216

We present a semi-analytic treatment of galactic winds within high-resolution, large-scale cosmological N -body simulations of a Λ cold dark matter (ΛCDM) universe. The evolution of winds is investigated by following the expansion of supernova-driven superbubbles around the several hundred thousand galaxies that form in an approximately spherical region of space with diameter 52  h ⁻¹ Mpc and mean density close to the mean density of the universe. We focus our attention on the impact of winds on the diffuse intergalactic medium. Initial conditions for mass loss at the base of winds are taken from Shu, Mo & Mao. Results are presented for the volume filling factor and the mass fraction of the intergalactic medium (IGM) affected by winds, and their dependence on the model parameters is carefully investigated. The mass-loading efficiency of bubbles is a key factor to determine the evolution of winds and their global impact on the IGM: the higher the mass loading, the later the IGM is enriched with metals. Galaxies with 10⁹ < M _★ < 10¹⁰ M_⊙ are responsible for most of the metals ejected into the IGM at   z = 3  , while galaxies with   M _★ < 10⁹ M_⊙   give a non-negligible contribution only at higher redshifts, when larger galaxies have not yet assembled. We find a higher mean IGM metallicity than Lyα forest observations suggest, and we argue that the discrepancy may be explained by the high temperatures of a large fraction of the metals in winds, which may not leave detectable imprints in absorption in the Lyα forest.  相似文献   

Galaxy groups at 0.3 ≤z≤ 0.55 – I. Group properties     

D. J. Wilman †  M. L. Balogh ‡  R. G. Bower  J. S. Mulchaey  A. Oemler  Jr    R. G. Carlberg  S. L. Morris  R. J. Whitaker 《Monthly notices of the Royal Astronomical Society》2005,358(1):71-87

The evolution of galaxies in groups may have important implications for the evolution of the star formation history of the Universe, since many processes which operate in groups may suppress star formation and the fraction of galaxies in bound groups grows rapidly between   z = 1  and the present day. In this paper, we present an investigation of the properties of galaxies in galaxy groups at intermediate redshift  ( z ∼ 0.4)  . The groups were selected from the Canadian Network for Observational Cosmology Redshift Survey (CNOC2) redshift survey as described by Carlberg et al., with further spectroscopic follow-up undertaken at the Magellan telescope in order to improve the completeness and depth of the sample. We present the data for the individual groups, and find no clear trend in the fraction of passive galaxies with group velocity dispersion and group concentration. We stack the galaxy groups in order to compare the properties of group galaxies with those of field galaxies at the same redshift. The groups contain a larger fraction of passive galaxies than the field, this trend being particularly clear for galaxies brighter than   M _{B J} < −20  in the higher velocity dispersion groups. In addition, we see evidence for an excess of bright passive galaxies in the groups relative to the field. In contrast, the luminosity functions of the star-forming galaxies in the groups and the field are consistent. These trends are qualitatively consistent with the differences between group and field galaxies seen in the local Universe.  相似文献   

Numerical simulations of the Hyades dynamics and the nature of the moving Hyades cluster     

Ya. O. Chumak  A. S. Rastorguev  S. J. Aarseth 《Astronomy Letters》2005,31(5):308-314

We present our numerical simulations of the dynamical evolution of the Hyades open cluster. The simulations were performed usinga modified NBODY6 algorithm that included tidal forces and a realistic orbit of the cluster in a gravitational field described by the Miyamoto-Nagai potential. Our goal was to study the nature of movingclu sters. We show that the stars that were earlier cluster members could be later identified within a sphere of 50 pc in diameter around the Sun. The number of such stars for the chosen initial mass and virial radius of the cluster does not exceed ten. The maximum space velocity of these stars relative to the core of the current cluster does not exceed 3 km s^?1. Our numerical simulations confirm the assumption that some of the moving clusters near the Sun could consist of stars that have escaped from open clusters in the course of their dynamical evolution.  相似文献   

Supermassive black hole demography: the match between the local and accreted mass functions     

F. Shankar  P. Salucci  G. L. Granato  G. De Zotti  L. Danese 《Monthly notices of the Royal Astronomical Society》2004,354(4):1020-1030

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Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution     

L. G. Althaus †  A. H. Córsico ‡  A. Gautschy  Z. Han  A. M. Serenelli ‡  J. A. Panei ‡ 《Monthly notices of the Royal Astronomical Society》2004,347(1):125-136

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