Mass segregation in young stellar clusters     

Ian A. Bonnell  & Melvyn B. Davies 《Monthly notices of the Royal Astronomical Society》1998,295(3):691-698

We investigate the evolutionary effect of dynamical mass segregation in young stellar clusters. Dynamical mass segregation acts on a time-scale of order the relaxation time of a cluster. Although some degree of mass segregation occurs earlier, the position of massive stars in rich young clusters generally reflects the cluster's initial conditions. In particular, the positions of the massive stars in the Trapezium cluster in Orion cannot be due to dynamical mass segregation, but indicate that they formed in, or near, the centre of the cluster. Implications of this for cluster formation and for the formation of high-mass stars are discussed.  相似文献   

Spectroscopic observations of the eclipsing polar MN Hya (RX J0929–24)     

Gavin Ramsay  & Peter J. Wheatley 《Monthly notices of the Royal Astronomical Society》1998,301(1):95-100

We present low–medium resolution optical spectroscopy of the eclipsing AM Her system MN Hya (RX J0929–24). We determine the magnetic field strength at the primary accretion region of the white dwarf to be 42 MG from the spacing of cyclotron features visible during π ∼ 0.4–0.7. From spectra taken during the eclipse we find that the secondary has an M3–4 spectral type. Combined with the eclipse photometry of Sekiguchi, Nakada &38; Bassett and an estimate of the interstellar extinction we find a distance of ∼300–700 pc. We find unusual line variations at π ∼ 0.9: Hα is seen in absorption and emission. This is at the same point in the orbital phase at which a prominent absorption dip is seen in soft X-rays.  相似文献   

An 'outside-in' outburst of Aql X–1     

T. Shahbaz  R. M. Bandyopadhyay  P. A. Charles  R. M. Wagner  P. Muhli  P. Hakala  J. Casares  & J. Greenhill 《Monthly notices of the Royal Astronomical Society》1998,300(4):1035-1040

We present optical spectroscopy and optical and infrared photometry of the neutron star soft X-ray transient Aql X–1 during its X-ray outburst of 1997 August. By modelling the X-ray, optical and IR light curves, we find a 3-d delay between the IR and X-ray rise times, analogous to the UV–optical delay seen in dwarf novae outbursts and black hole X-ray transients. We interpret this delay as the signature of an 'outside-in' outburst, in which a thermal instability in the outer disc propagates inward. This outburst is the first of this type definitively identified in a neutron star X-ray transient.  相似文献   

The expulsion and retention of dust grains by galactic discs     

J. I. Davies  P. Alton  S. Bianchi  & M. Trewhella 《Monthly notices of the Royal Astronomical Society》1998,300(4):1006-1014

We have constructed a numerical model of a galaxy that consists of a stellar, gas and dust disc imbedded within a dark halo. We have used this model to assess the radiation, gravitational and viscous forces on dust grains and to trace their motion through the interstellar medium over a period of 10⁹ yr. We conclude that the disc opacity is a crucial factor in understanding the motion of the grains. Large grains (≈0.1 μm) with low disc opacity will lead to dust expulsion from the stellar disc, while high opacity leads to dust retention. Reasonable disc opacities lead to the recycling of the larger grains from the outer to the inner regions of the galaxy. The larger grains travel at higher velocities than small grains (0.01−0.001 μm), and so the smaller grains remain relatively close to their formation sites. Dust can 'leak' out over the entire surface of the disc because of the imbalance of radiation and gravitational forces. The dust is dynamically coupled to the gas and so although the gas lags behind the dust it is carried along with it. This explains the close correlation between the far-infrared emission from dust and the gas column density. We use a simple analytical model to show how the dust mass of a galaxy may evolve with time and how a significant fraction (90 per cent) of the total dust mass produced may have been expelled into the intergalactic medium.  相似文献   

Numerical simulations of protostellar encounters — II. Coplanar disc–disc encounters     

S. J. Watkins  A. S. Bhattal  H. M. J. Boffin  N. Francis  & A. P. Whitworth 《Monthly notices of the Royal Astronomical Society》1998,300(4):1205-1213

It is expected that an average protostar will undergo at least one impulsive interaction with a neighbouring protostar whilst a large fraction of its mass is still in a massive, extended disc. Such interactions must have a significant impact upon the evolution of the protostars and their discs.   We have carried out a series of simulations of coplanar encounters between two stars, each possessing a massive circumstellar disc, using an SPH code that models gravitational, hydrodynamic and viscous forces. We find that during a coplanar encounter, disc material is swept up into a shock layer between the two interacting stars, and the layer then fragments to produce new protostellar condensations. The truncated remains of the discs may subsequently fragment; and the outer regions of the discs may be thrown off to form circumbinary disc-like structures around the stars. Thus coplanar disc–disc encounters lead efficiently to the formation of multiple star systems and small- N clusters, including substellar objects.  相似文献   

Line emission from accretion discs around black holes: the analytic approach     

Andrej ?ade?  Claudio Fanton  Massimo Calvani 《New Astronomy》1998,3(8):528-654

The broad X-ray iron line observed in many active galactic nuclei spectra is thought to originate from the accretion disc surrounding the putative supermassive black hole. We show here how to perform the analytical integration of the geodesic equations that describe the photon trajectories in the general case of a rotating black hole (Kerr metric), in order to write a fast and efficient numerical code for modelling emission line profiles from accretion discs.  相似文献   

影响流域土壤流失的降水量的PPAR(K)预测模型     

李祚泳  邓新民  侯宇光 《成都信息工程学院学报》1998,(2)

介绍了投影寻踪自回归（ＰＰＡＲ（Ｋ））的基本思想及其算法。用ＰＰＡＲ（Ｋ）和均生函数（ＭＧＦ）两种方法对泸州市和北碚市降水量的时间序列进行了建模预测。结果表明ＰＰＡＲ（Ｋ）模型具有较高的稳定性和预测精度。  相似文献   

信息量法在西宁市斜坡稳定性评价中的应用   总被引：11，自引：1，他引：10  

毕海良 《水文地质工程地质》1998,25(4):25-27

本文选定西宁市东川弱侧丘陵前缘做为评价对象,采用二态变量信息法,对斜皮稳定性进行试评价。通过本次尝试性计算评价,与实际情况对比检验,其准确率达到８９％。故本方法在斜坡稳定性评价中较为实用。  相似文献   

滞后补给权函数：降雨补给潜水滞后性处理方法   总被引：16，自引：0，他引：16  

陈崇希 《水文地质工程地质》1998,25(6):22-24

本文分析了当前数值模型中处理降雨入渗补给潜水方法中存在的问题,提出一种能刻画滞后补给且使用方便的方法－滞后补给权函数法。  相似文献   

滑坡临界暴雨强度   总被引：29，自引：1，他引：28  

柳源 《水文地质工程地质》1998,25(3):43-45

本文介绍了几个主要暴雨滑坡集中区的临界暴雨强度,分析了各地临界暴雨强度不同的主要原因。指出前期降雨对滑坡滑动是否有明显影响,取决于滑体岩土性质及滑坡形成机制等多种因素,不可一概而论。  相似文献