Shock oscillation model for quasi-periodic oscillations in stellar mass and supermassive black holes

We numerically examine centrifugally supported shock waves in 2D rotating accretion flows around a stellar mass  (10 M_⊙)  and a supermassive  (10⁶ M_⊙)  black holes over a wide range of input accretion rates of     . The resultant 2D shocks are unstable with time and the luminosities show quasi-periodic oscillations (QPOs) with modulations of a factor of 2–3 and with periods of a tenth of a second to several hours, depending on the black hole masses. The shock oscillation model may explain the intermediate frequency QPOs with 1–10 Hz observed in the stellar mass black hole candidates and also suggest the existence of QPOs with the period of hours in active galactic nuclei. When the accretion rate     is low, the luminosity increases in proportion to the accretion rate. However, when     greatly exceeds the Eddington critical rate     , the luminosity is insensitive to the accretion rate and is kept constantly around  ∼3 L _E  . On the other hand, the mass-outflow rate     increases in proportion to     and it amounts to about a few per cent of the input mass-flow rate.     

黑洞吸积理论及其天体物理学应用的近期发展(Ⅱ)

黑洞吸积理论是天体物理学的一个基础理论,是认识许多高能天体系统如活动星系核、黑洞X射线双星,以及伽马暴等的重要物理基础.该文评述近年来黑洞吸积理论尤其是径移主导吸积流模型(advection-dominated accretion flow)及其变种的主要发展,并介绍该理论在银河系中心、低光度活动星系核、黑洞X射线双星等方面的应用.共分为两篇,该文是第2篇,内容是关于黑洞热吸积流理论在低光度活动星系核以及黑洞X射线双星方面的应用.     

Iron line profiles and self-shadowing from relativistic thick accretion discs

We present Fe Kα line profiles from and images of relativistic discs with finite thickness around a rotating black hole using a novel code. The line is thought to be produced by iron fluorescence of a relatively cold X-ray-illuminated material in the innermost parts of the accretion disc and provides an excellent diagnostic of accretion flows in the vicinity of black holes. Previous studies have concentrated on the case of a thin, Keplerian accretion disc. This disc must become thicker and sub-Keplerian with increasing accretion rates. These can affect the line profiles and in turn can influence the estimation of the accretion disc and black hole parameters from the observed line profiles. We here embark on, for the first time, a fully relativistic computation which offers key insights into the effects of geometrical thickness and the sub-Keplerian orbital velocity on the line profiles. We include all relativistic effects such as frame-dragging, Doppler boost, time dilation, gravitational redshift and light bending. We find that the separation and the relative height between the blue and red peaks of the line profile diminish as the thickness of the disc increases. This code is also well suited to produce accretion disc images. We calculate the redshift and flux images of the accretion disc and find that the observed image of the disc strongly depends on the inclination angle. The self-shadowing effect appears remarkable for a high inclination angle, and leads to the black hole shadow being in this case, completely hidden by the disc itself.     

Primordial black holes

Primordial black holes (PBHs) are a profound signature of primordial cos-mological structures and provide a theoretical tool to study nontrivial physics of the early Universe. The mechanisms of PBH formation are discussed and observational constraints on the PBH spectrum, or effects of PBH evaporation, are shown to re-strict a wide range of particle physics models, predicting an enhancement of the ul-traviolet part of the spectrum of density perturbations, early dust-like stages, first or-der phase transitions and stages of superheavy metastable particle dominance in the early Universe. The mechanism of closed wall contraction can lead, in the inflation-ary Universe, to a new approach to galaxy formation, involving primordial clouds of massive BHs created around the intermediate mass or supermassive BH and playing the role of galactic seeds.     

北秦岭清岩沟镍-钼矿床成矿特征及成因

经野外调研和室内研究发现,位于商州市大荆镇北的清岩沟镍-钼矿床赋存于庙湾组下部黑色岩系中,岩系由绢云斜长石英千枚岩、黑云斑点状二云母千枚岩、石墨化绢云千枚岩、白云母细晶大理岩-碳质白云岩、含石墨石英透辉透闪岩、含钛方解-石英片岩等组成,含Mo、Ni、Ti、Cu、Pb、Zn、P及碳质高。宏观及微观地质特征表明,岩石经历了区域变质变形、后期强烈韧-脆性剪切构造作用叠加、改造。正是这种地质过程导致Mo、Ni等成矿元素在沉积期形成之后,发生迁移、沉淀,形成硫化物型镍、钼矿化,矿(化)体就位于岩系强烈揉皱与膨大的片理化带、赋存于强变形的刚性与塑性构造体接触带。研究表明区内的岩脉与矿化关系不明显。最后认为,清岩沟镍-钼矿床为黑色岩系容矿的层控型沉积-变质叠加-韧脆性构造改造的后生热液成因矿床。     

南秦岭千家坪钒矿床地质地球化学特征与钒的富集规律

千家坪钒矿床产于南秦岭下寒武统水沟口组(缀1sh)黑色岩系中,该黑色岩系由黑色含炭硅质岩、含炭硅质岩夹泥岩和泥岩等组成。钒矿体呈层状产出,矿石以黑色硅质岩夹泥岩型为主,含钒矿物主要为钒云母。黑色岩系岩石主要成分为SiO2、Al2O3、K2O等,富集TFe、Ba、Zn、P、Cu、Ni、Cr、Sr、Zr、Ag、Ti、Mn、V等多种元素。黑色岩系n(V)/n(Cr)=5.92～30.64、n(V)/n(V+Ni)=0.88～0.99、δU1,判断其为缺氧沉积环境。黑色硅质岩n(SiO2)/n(Al2O3)=238.81,U/Th1以及δ30Si=-0.1‰～0.5‰、δ18O=20.2‰～25.8‰,判断其为半深海滞留沉积盆地热水沉积成因。泥岩n(SiO2)/n(Al2O3)=5.69,n(Al)/n(Al+Fe+Mn)=0.63,n(Si)/n(Si+Al+Fe)=0.74～0.76判断其物源为陆源,但受到热水作用影响。钒矿化受下寒武世古隆起边缘断陷滞留盆地中形成的黑色岩系层位所控制。钒明显趋向在炭硅质岩所夹的泥岩或硅质岩附近的泥岩中富集,在炭硅质岩夹泥岩段向泥岩段过渡层位,常常含结核,钒元素含量达到峰值,其他Cu、Pb、Zn、As、W、Mo等元素富集规律与V元素基本一致。该矿床成矿物质主要来源于深部热水,泥岩的吸附作用对钒的富集具有重要作用。综合地质、地球化学特征,认为该矿床为热水喷流沉积成因。