塔里木盆地原油孢粉集合   总被引：5，自引：2，他引：3  

江德昕  杨惠秋 《沉积学报》2000,18(1):80-88

记述了塔里木盆地 44个原油样品中发现的孢子花粉化石 83属 1 6 3种 基于原油孢粉集合组成的研究,探讨了塔北、库车、喀什和叶城四个含油区油源岩的时代和层位 并根据孢粉化石的颜色鉴定了油源岩的成熟度。研究结果表明,研究区石炭系、三叠系和侏罗系油源岩都是成熟的油源岩。此外,还详细介绍了从原油中萃取孢子花粉和藻类化石的方法。  相似文献   

塔里木盆地中高氮天然气的成因及其与天然气聚集的关系   总被引：2，自引：0，他引：2  

《沉积学报》2000,18(4)

塔里木盆地塔北和塔中地区的海相腐泥型天然气,N2含量较高,尤其是湿气,N2含量分布在10.1％～36.2％,而干气的N2含量则低于10％,即湿气的N2含量高于干气的N2含量。同是下古生界寒武－奥陶系来源的海相腐泥型天然气,为什么湿气和干气的氮气含量相差如此之大?根据与氮气相伴生的烃类气体、非烃气体及稀有气体的组份及同位素特征,认为塔里木盆地的中高氮天然气属于有机成因,来源于下古生界海相烃源岩。文章还提出塔北和塔中地区湿气和干气N2含量差异与源岩的演化程度和圈闭的捕获条件有关。  相似文献   

The extended rotation curve and the dark matter halo of M33     

Edvige Corbelli  Paolo Salucci 《Monthly notices of the Royal Astronomical Society》2000,311(2):441-447

We present the 21-cm rotation curve of the nearby galaxy M33 out to a galactocentric distance of 16 kpc (13 disc scalelengths). The rotation curve keeps rising out to the last measured point and implies a dark halo mass ≳5×10¹⁰ M_⊙. The stellar and gaseous discs provide virtually equal contributions to the galaxy gravitational potential at large galactocentric radii, but no obvious correlation is found between the radial distribution of dark matter and the distribution of stars or gas.
Results of the best fit to the mass distribution in M33 picture a dark halo which controls the gravitational potential from 3 kpc outward, with a matter density which decreases radially as R ^−1.3. The density profile is consistent with the theoretical predictions for structure formation in hierarchical clustering cold dark matter (CDM) models, and favours lower mass concentrations than those expected in the standard cosmogony.  相似文献   

Non-linear density evolution from an improved spherical collapse model     

Sunu Engineer  Nissim Kanekar  T. Padmanabhan 《Monthly notices of the Royal Astronomical Society》2000,314(2):279-289

We investigate the evolution of non-linear density perturbations by taking into account the effects of deviations from spherical symmetry of a system. Starting from the standard spherical top hat model in which these effects are ignored, we introduce a physically motivated closure condition which specifies the dependence of the additional terms on the density contrast, δ . The modified equation can be used to model the behaviour of an overdense region over a sufficiently large range of δ . The key new idea is a Taylor series expansion in (1/ δ ) to model the non-linear epoch. We show that the modified equations quite generically lead to the formation of stable structures in which the gravitational collapse is halted at around the virial radius. The analysis also allows us to connect up the behaviour of individual overdense regions with the non-linear scaling relations satisfied by the two-point correlation function.  相似文献   

The local density of matter mapped by Hipparcos     

Johan Holmberg  Chris Flynn 《Monthly notices of the Royal Astronomical Society》2000,313(2):209-216

We determine the velocity distribution and space density of a volume-complete sample of A and F stars, using parallaxes and proper motions from the Hipparcos satellite. We use these data to solve for the gravitational potential vertically in the local Galactic disc, by comparing the Hipparcos measured space density with predictions from various disc models. We derive an estimate of the local dynamical mass density of 0.102±0.010 pc⁻³, which may be compared with an estimate of 0.095 M_⊙ pc⁻³ in visible disc matter. Our estimate is found to be in reasonable agreement with other estimates by Crézé et al. and Pham, also based on Hipparcos data. We conclude that there is no compelling evidence for significant amounts of dark matter in the disc.  相似文献   

A population of very young brown dwarfs and free-floating planets in Orion     

P. W. Lucas  P. F. Roche 《Monthly notices of the Royal Astronomical Society》2000,314(4):858-864

We describe the results of a very deep imaging survey of the Trapezium cluster in the IJH bands, using the UKIRT high-resolution camera UFTI. Approximately 32 per cent of the 515 point sources detected are brown dwarf candidates, including several free-floating objects with masses below the deuterium-burning (planetary) threshold at 0.013 M_⊙, which are detectable because of their extreme youth. We have confidence that almost all the sources detected are cluster members, since foreground contamination is minimal in the 33-arcmin² area surveyed, and the dense backdrop of OMC-1 obscures all background stars at these wavelengths. Extinction is calculated from the ( J − H ) colours, permitting accurate luminosity estimates, and temperatures are derived from the dereddened ( I − J ) colours. There is some evidence for a cut-off in the luminosity function below the level corresponding to several Jupiter masses, which may represent the bottom end of the initial mass function . Since star formation is complete in the Trapezium, this limit could have wide significance, if confirmed. However, it could well be an effect of the dispersal of the molecular cloud by the central O-type stars, a process for which the time-scale will vary between star formation regions.  相似文献   

Optical properties of the carbon dust grains in the envelopes around asymptotic giant branch stars     

Kyung-Won Suh 《Monthly notices of the Royal Astronomical Society》2000,315(4):740-750

We have investigated the optical properties of the carbon dust grains in the envelopes around carbon-rich asymptotic giant branch stars, paying close attention to the infrared observations of the stars and the laboratory-measured optical data of the candidate dust grain materials. We have compared the radiative transfer model results with the observed spectral energy distributions of the stars including IRAS Point Source Catalog and IRAS Low Resolution Spectrograph data. We have deduced an opacity function of amorphous carbon dust grains from model fitting with infrared carbon stars. From the opacity function, we have derived the optical constants of the AMC grains. The optical constants satisfy the Kramers–Kronig relation and produce the opacity function that fits the observations of infrared carbon stars better than previous works in the wide wavelength range 1–1000 μm. We have used simple mixtures of the AMC and silicon carbide grains for modelling. We have compared the contributions that AMC and SiC grains make to the opacity for the cases of simple mixtures of them and spherical core–mantle type grains consisting of a SiC core and an AMC mantle .  相似文献   

The cosmological dependence of galactic specific angular momenta     

Vincent Eke  †  George Efstathiou  Lisa Wright 《Monthly notices of the Royal Astronomical Society》2000,315(2):L18-L22

Hydrodynamical simulations of galaxy formation in spatially flat cold dark matter (CDM) cosmologies with and without a cosmological constant (Λ) are described. A simple star formation algorithm is employed and radiative cooling is allowed only after redshift z =1 so that enough hot gas is available to form large, rapidly rotating stellar discs if angular momentum is approximately conserved during collapse. The specific angular momenta of the final galaxies are found to be sensitive to the assumed background cosmology. This dependence arises from the different angular momenta contained in the haloes at the epoch when the gas begins to collapse and the inhomogeneity of the subsequent halo evolution. In the Λ-dominated cosmology, the ratio of stellar specific angular momentum to that of the dark matter halo (measured at the virial radius) has a median value of ∼0.24 at z =0. The corresponding quantity for the Λ=0 cosmology is over three times lower. It is concluded that the observed frequency and angular momenta of disc galaxies pose significant problems for spatially flat CDM models with Λ=0 but may be consistent with a Λ-dominated CDM universe.  相似文献   

Sputtering in the outflows of cool stars     

Carl Covatto  Per A. Aannestad 《Monthly notices of the Royal Astronomical Society》2000,318(1):67-72

Radiation pressure acts to accelerate dust grains and, by transfer of momentum through collisions with the gas, drives the outflows of late-type stars. Some of these dust–gas collisions may be energetic enough to remove atoms from the dust grains. From an assumed initial size distribution for the dust grains, the method of Krüger et al. is used to study the evolution of a sample of spherical amorphous carbon grains under conditions typical of a late-type star. The size distribution of dust grains is presented for various sets of model parameters. One set of models assumes an initial Mathis, Rumpl & Nordsieck (MRN) distribution for the dust grains. The high-luminosity ( L ∗), high-effective temperature ( T _eff) set of parameters has a terminal velocity ( v _term) that is near, but above , the upper limit of observed outflow velocities for carbon stars (∼30 km s⁻¹ for the assumed ̇ of 5×10⁻⁶ M_⊙ yr⁻¹). The low L ∗, T _eff model has a v _term that lies near, but below , the upper limit of observed velocities. A significant amount of sputtering occurs in the high L ∗, T _eff model with ∼40 per cent of the grain mass sputtered. About ∼1 per cent of the dust mass is sputtered in the low L ∗, T _eff. Another set of models assumes that the dust forms with a log-normal distribution. Here, v _term is nearly the same for the high L ∗, T _eff model as for the low L ∗, T _eff model. This is a result of the large amount of dust mass loss (∼75 per cent) by sputtering in the high L ∗, T _eff model.  相似文献   

Constraining the cosmic equation of state from old galaxies at high redshift     

J. A. S. Lima  J. S. Alcaniz 《Monthly notices of the Royal Astronomical Society》2000,317(4):893-896

New limits on the cosmic equation of state are derived from age measurements of three recently reported old high-redshift galaxies (OHRG). The results are based on a flat Friedmann–Robertson–Walker (FRW) type cosmological model driven by non-relativistic matter plus a smooth component parametrized by its equation of state p _x ωρ _x ( ω −1). The range of ω is strongly dependent on the matter density parameter. For Ω_M∼0.3, as indicated from dynamical measurements, the age estimates of the OHRG restrict the cosmic parameter to ω −0.27. However, if Ω_M is the one suggested by some studies of field galaxies, i.e., Ω_M≃0.5, only a cosmological constant ( ω =−1) may be compatible with these data.  相似文献