The fraction of galaxies that contain active nuclei and their accretion rates

We investigate the relationship between the present-day optical luminosity function of galaxies and the X-ray luminosity function of Seyfert 1s to determine the fraction of galaxies that host Seyfert 1 nuclei and their Eddington ratios. The local type 1 active galactic nuclei (AGN) X-ray luminosity function is well reproduced if ∼1 per cent of all galaxies are type 1 Seyferts which have Eddington ratios of ∼10⁻³. However, in such a model the X-ray luminosity function is completely dominated by AGN in E and S0 galaxies, contrary to the observed mix of Seyfert host galaxies. To obtain a plausible mix of AGN host galaxy morphologies requires that the most massive black holes in E and S0 galaxies accrete with lower Eddington ratios, or have a lower incidence of Seyfert activity, than the central black holes of later-type galaxies.     

Peculiarities of the UV continuum energy distribution for T Tauri stars

In the UV spectra of BP Tau, GW Ori, T Tau, and RY Tau obtained with the Hubble Space Telescope, we detected an inflection near 2000 Å in the F _λ ^c (λ) curve that describes the continuum energy distribution. The inflection probably stems from the fact that the UV continuum in these stars consists of two components: the emission from an optically thick gas with T<8000 K and the emission from a gas with a much higher temperature. The total luminosity of the hot component is much lower than that of the cool component, but the hot-gas radiation dominates at λ<1800 Å. Previously, other authors have drawn a similar conclusion for several young stars from low-resolution IUE spectra. However, we show that the short-wavelength continuum is determined from these spectra with large errors. We also show that, for three of the stars studied (BP Tau, GW Ori, and T Tau), the accretion-shock radiation cannot account for the observed dependence F _λ ^c (λ) in the ultraviolet. We argue that more than 90% of the emission continuum in BP Tau at λ>2000 Å originates not in the accretion shock but in the inner accretion disk. Previously, a similar conclusion was reached for six more classical T Tau stars. Therefore, we believe that the high-temperature continuum can be associated with the radiation from the disk chromosphere. However, it may well be that the stellar chromosphere is its source.     

X-ray emission from accretion disks in active galactic nuclei

We constructed a grid of relativistic models for standard high-relative-luminosity accretion α-disks around supermassive Kerr black holes (BHs) and computed X-ray spectra for their hot, effectively optically thin inner parts by taking into account general-relativity effects. They are known to be heated to high (～10⁶–10⁹ K) temperatures and to cool down through the Comptonization of intrinsic thermal radiation. Their spectra are power laws with an exponential cutoff at high energies; i.e., they have the same shape as those observed in active galactic nuclei (AGNs). Fitting the observed X-ray spectra of AGNs with computed spectra allowed us to estimate the fundamental parameters of BHs (their mass and Kerr parameter) and accretion disks (luminosity and inclination to the line of sight) in 28 AGNs. We show that the Kerr parameter for BHs in AGNs is close to unity and that the disk inclination correlates with the Seyfert type of AGN, in accordance with the unification model of activity. The estimated BH masses M_x are compared with the masses M_rev determined by the reverberation mapping technique. For AGNs with luminosities close to the Eddington limit, these masses agree and the model under consideration may be valid for them. For low-relative-luminosity AGNs, the differences in masses increase with decreasing relative luminosity and their X-ray emission cannot be explained by this model.     

赣东北前寒武纪港边杂岩体的岩浆混合（和）作用及其地质意义

赣东北地区沿江绍断裂北缘和江南造山带南侧有大量的前寒武纪火山侵入杂岩呈带状分布,主要由大面积的陆相火山岩和若干长英质镁铁质火成杂岩体组成,后者中出露面积最大的港边杂岩体在填图尺度上可划分为长英质岩、镁铁质岩和过渡性岩3大组成部分,长英质岩颗粒锆石U_Pb谐和不一致曲线上交点年龄为822±4Ma,代表杂岩体中岩浆混合作用发生的时间。港边岩体中长英质岩石的Nd模式年龄为1·49~1·68Ga,镁铁质岩中玄武质岩石为1·51~2·21Ga,辉长岩的Nd模式年龄与玄武质岩石基本相同,为1·54~2·13Ga,经计算的过渡性岩石的Nd模式年龄为1·58~1·90Ga,因此认为镁铁质岩石从源区分离的时间要远早于长英质岩石,而过渡性岩石含有前两个端员岩浆相互混合(和)的信息。长英质岩石的εNd(t=822Ma)值为-0·8~-4·4,87Sr/86Sr(822)比值为0·70368~0·70549;玄武质岩石的εNd(822)值为-2·6~+2·3,87Sr/86Sr(822)比值为0·70387~0·70527,这反映了镁铁质岩浆的源区接近总地球,长英质岩浆则来自具壳幔混合性质的EMⅠ型地幔的源区。可以推测,赣东北前寒武纪也曾发生过岩浆底侵作用。底侵作用对港边火成杂岩体岩浆的形成起着重要的作用。底侵于壳幔边界的玄武质岩浆使地壳熔融形成长英质岩浆并聚集于浅部岩浆房。随着长英质岩浆房降温,长英质岩浆的结晶度和粘度增加,其物理状态发生液态→(固+液)混合态→固态的变化;当玄武质岩浆穿透下地壳并不断进入物理状态变化的长英质岩浆房时,持续地发生两种岩浆的化学混合作用或两岩浆的机械混合作用或玄武质岩浆的侵入,其混合作用的时间以长英质岩锆石的U_Pb谐和不一致曲线上交点年龄822±4Ma界定。根据Nd模式年龄(tDM)和Nd富集系数(fSm/Nd)分布特征,可以确定中元古代江南造山带为太古宙扬子古陆核的横向增生体,而新元古代陆相火山侵入杂岩带则横向增生于江南造山带南缘。至此,扬子古陆横向增生作用结束,开始与华夏古陆拼贴,包括港边火成杂岩体在内的新元古代火山侵入杂岩带则成为两古陆连结的纽带。     

新疆晚古生代大陆边缘成矿系统与成矿区带初步探讨

新疆地处中亚成矿域的中段，古生代大陆边缘增生明显、构造和岩浆活动强烈、矿产资源丰富。古生代大陆边缘成矿作用主要集中在两个时期，即以阿尔泰南缘为主的早中泥盆世和以天山为主的早石炭世。本文在综合研究及与境外对比的基础上，按照北疆地区晚古生代大陆边缘的构造动力学和成矿特征，将研究区大陆边缘成矿系统划分为：活动大陆边缘海相火山岩-盆地流体成矿系统，活动大陆边缘火山岛弧-岩浆活动成矿系统和被动大陆边缘沉积盆地-热水活动成矿系统三类。同时对形成于大陆边缘的成矿区带进行划分，主要包括：阿勒泰南缘晚古生代活动大陆边缘块状硫化物成矿带；阿尔泰南缘-东准噶尔活动大陆边缘卡拉先格尔岛弧斑岩铜金成矿带；东天山晚古生代活动大陆边缘铜钼锌成矿区带；西准噶尔洋内弧斑岩-浅成低温热液铜金成矿区带；西天山（伊犁地块）活动大陆边缘金铜成矿区带；塔里木板块被动大陆边缘沉积型铅锌成矿带。本文认为大陆增生与成矿作用的关系是矿床学和成矿系统研究的重要内容，成矿区带是成矿系统发生成矿作用的响应，而成矿系统是成矿区带形成的本质。     

On the Dynamics of Dust Grains in a Hierarchical Environment

Most main sequence stars are binaries or higher multiplicity Systems and it appears that at birth most stars have circumstellar disks. It is commonly accepted that planetary systems arise from the material of these disks; consequently, binary and multiple systems may have a main role in planet formation. In this paper, we study the stage of planetary formation during which the particulate material is still dispersed as centimetre-to-metre sized primordial aggregates. We investigate the response of the particles, in a protoplanetary disk with radius R_D = 100 AU around a solar-like star, to the gravitational field of bound perturbing companions in a moderately wide (300–1600 AU) orbit. For this purpose, we have carried out a series of simulations of coplanar hierarchical configurations using a direct integration code that models gravitational and viscous forces. The massive protoplanetary disk is around one of the components of the binary. The evolution in time of the dust sub-disk depends mainly on the nature (prograde or retrograde) of the relative revolution of the stellar companion, and on the temperature and mass of the circumstellar disk. Our results show that for binary companions near the limit of tidal truncation of the disk, the perturbation leads to an enhanced accretion rate onto the primary, decreasing the lifetime of the particles in the protoplanetary disk with respect to the case of a single star. As a consequence of an enhanced accretion rate the mass of the disk decreases faster, which leads to a longer resultant lifetime for particles in the disk. On the other hand, binary companions may induce tidal arms in the dust phase of protoplanetary disks. Spiral perturbations with m = 1 may increase in a factor 10 or more the dust surface density in the neighbourhood of the arm, facilitating the growth of the particles. Moreover, in a massive disk (0.01M⊙) the survival time of particles is significantly shorter than in a less massive nebula (0.001M⊙) and the temperature of the disk severely influences the spiral-in time of particles. The rapid evolution of the dust component found in post T Tauri stars can be explained as a result of their binary nature. Binarity may also influence the evolution of circumpulsar disks. This revised version was published online in July 2006 with corrections to the Cover Date.     

Disc structure around strongly magnetic accretors: a full disc solution with buoyancy diffusivity

A full numerical solution is found for the effect of a strongly magnetic star on its accretion disc, for the case of magnetic buoyancy diffusion. As in the previously considered case of turbulent diffusion, the disc becomes disrupted when magnetic and viscous stresses become comparable. A magnetically induced temperature elevation leads to electron scattering opacity and radiation pressure becoming significant far from the stellar surface, with consequent viscous instability and vertical disruption of the disc. This, together with the previous turbulent case, suggests that such a disruption mechanism owing to strongly magnetic accretors is generally operable.     

Stream overflow and dwarf nova eruptions

We consider the effects of accretion stream overflow on the viscous dynamics of accretion discs in dwarf novae. If the stream from the secondary star is geometrically thick enough, some fraction of its material can flow over and under the disc. The mass and specific angular momentum of the stream are then deposited not only at the point of collision with the outer disc, but also at those radii in the inner disc with geometric heights that are large enough to intercept the residual stream, or near the radius where the disc has the same specific angular momentum as the stream. The overflowing stream can alter the behaviour of heating fronts and cooling fronts in the disc. If the mass fraction of the overflowing stream is of order tens of per cent, the deposition of mass in the inner parts of the disc is sufficient to change the character of the eruption light curves significantly.     

An 'outside-in' outburst of Aql X–1

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.     

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

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.