Dissipative accretion flows around a rotating black hole     

Santabrata Das  Sandip K. Chakrabarti 《Monthly notices of the Royal Astronomical Society》2008,389(1):371-378

We study the dynamical structure of a cooling dominated rotating accretion flow around a spinning black hole. We show that non-linear phenomena such as shock waves can be studied in terms of only three flow parameters, namely the specific energy     , the specific angular momentum (λ) and the accretion rate     of the flow. We present all possible accretion solutions. We find that a significant region of the parameter space in the     plane allows global accretion shock solutions. The effective area of the parameter space for which the Rankine–Hugoniot shocks are possible is maximum when the flow is dissipation-free. It decreases with the increase of cooling effects and finally disappears when the cooling is high enough. We show that shock forms further away when the black hole is rotating compared to the solution around a Schwarzschild black hole with identical flow parameters at a large distance. However, in a normalized sense, the flow parameters for which the shocks form around the rotating black holes are produced shocks closer to the black hole. The location of the shock is also dictated by the cooling efficiency in that higher the accretion rate     , the closer is the shock location. We believe that some of the high-frequency quasi-periodic oscillations may be due to the flows with higher accretion rate around the rotating black holes.  相似文献   

Solar Type III Bursts and the Generation of Backward Langmuir Wave     

Yu Huang  Guang-li Huang 《Chinese Astronomy and Astrophysics》2008,32(2):178-185

It is generally believed that the conversion of Langmuir wave (LW) to electromagnetic wave is the generating mechanism of solar type III bursts. The Langmuir wave can be easily excited by the instability of the electron-beam current, and the interaction of the forward and backward Langmuir waves is considered to be the cause for the second harmonic of a type III burst, but, so far, the dispersion equation and generating mechanism of the backward Langmuir wave have not yet been thoroughly studied. For the equation of two-stream instability with temperature included, an analytical solution is derived. It is found that the dispersion relation of the forward LW strongly depends on the beam-current speed, while that of the backward LW depends only on the thermal velocity, when the other parameters are fixed. These analytical results are partially confirmed by particle-in-cell (PIC) simulations. With the PIC simulation, the generating mechanism of the backward LW is studied, and it is revealed that the backward LW can not be excited directly by the electron-beam current, and that its energy is obtained basically from the scattering of the forward LW. However, the electron-beam current does cause a direct amplification of the second harmonic of the forward LW.  相似文献   

Calculation of the Intensity Ratio and Intrinsic Redshift Ratio of the Cerenkov Iron K_α and K_β Lines and Its Possible Application in the Study of AGNs     

Dang-bo Liu  Lei Chen  Jun-han You 《Chinese Astronomy and Astrophysics》2008

We have pointed out that, when thermal relativistic electrons with an isotropic velocity distribution move through a region of dense gas or impinge upon its surface, the Cerenkov effect will produce a particular kind of atomic or ionic emission line, which we have called the “Cerenkov line-like radiation”. This prediction for the optical wavebands has been verified by laboratory experiments. In this paper, we extend this line-like radiation theory to the X-ray waveband and give the basic formulae for calculating the intensity ratio and intrinsic redshift ratio of the Cerenkov iron K_α and K_β lines, for different ionization orders of iron. Potential application of this calculated result may be found in the study of AGNs. The recent observations of NGC3783 show that besides the iron K_α line at ∼6.4 keV, there is also a very strong iron Kβ line at ∼7.0 keV, and that the ratio of equivalent widths between the two is anomalous: EWK_α/EWK_β ≈ 3.43. It is difficult to explain this by the conventional mechanism of “photoelectric absorption-fluorescence emission”. We suggest that the mechanism of Cerenkov line-like radiation can provides a way of solving this puzzle. Besides, we expect that the calculated intrinsic redshift ratio of Cerenkov iron K_α and K_β lines could be tested in future observations. If our suggestion is further supported by observations, then our view on the physical environment around the central massive black hole of an AGN will be greatly modified: the activity becomes more energetic and violent, and the gas, much denser than previously thought.  相似文献   

A possible disk mechanism for the 23-day QPO in Mkn 501     

J.H. Fan  F.M. Rieger  T.X. Hua  U.C. Joshi  J. Li  Y.X. Wang  J.L. Zhou  Y.H. Yuan  J.B. Su  Y.W. Zhang 《Astroparticle Physics》2008,28(6):508-515

  相似文献   

Nonlinear evolution of Tayler unstable equilibrium states     

D. Elstner  A. Bonanno  G. Rüdiger 《Astronomische Nachrichten》2008,329(7):717-721

We investigate the nonlinear evolution of Tayler unstable toroidal fields in a disk geometry, by numerical simulations. We consider non‐rotating and rigid rotating disks, with different radial field profiles. The initial configuration is in equilibrium, which is achieved by a pressure gradient or an external potential force. The nonlinear evolution of the system leads to a stable equilibrium with a current free toroidal field. Only for the fast rotating case we could preserve a ring type structure of the toroidal field. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

东营凹陷下第三系层序地层研究与隐蔽油气藏预测   总被引：18，自引：3，他引：15  

张德武  冯有良  邱以钢  闵伟  郭玉新  赵乐强  向立宏 《沉积学报》2004,22(1):67-72

应用层序地层学理论,利用地震、测井、岩心和分析化验资料,建立了东营凹陷下第三系层序界面识别标志,把东营凹陷下第三系划分为 1个超层序组,4个超层序,10个层序,进行体系域划分,建立了东营凹陷下第三系层序地层格架。构造坡折带是指由同沉积构造长期活动引起的沉积斜坡明显突变的地带,对盆地充填的可容纳空间和沉积作用可产生重要影响。通过层序地层格架与构造坡折带的研究,建立东营凹陷层序发育模式。受构造坡折带控制的层序低位域砂体和湖侵体系域砂体,成藏条件良好,最有利于形成隐蔽油气藏。  相似文献   

月球资源探测信息的管理与可视化探讨   总被引：1，自引：0，他引：1  

吴冲龙  毛小平  田宜平  张夏林  翁正平 《地质科技情报》2004,23(4):15-18

在中国未来的月球探测计划中,可能获取的月球表层数据包括地形、地貌、岩层、土壤、资源、环境以及各种相关的结构、物质成分数据。这些数据既有空间数据,也有属性数据。为了实现月球资源探测工作信息化,可以借鉴“数字地球”的理念并采用“多S”结合与集成化技术,对所获取的海量月球表层数据进行一体化存贮管理,构建一个“数字月球”并实现其空间数据和属性数据之间的双向查询检索,以及对表层复杂结构信息分析的可视化。  相似文献   

海上油藏勘探经济评价方法——以胜利滩海地区为例     

韩丽 《地质论评》2019,65(Z1):321-322

正油气勘探经济评价是勘探项目可行性研究的重要组成部分,在此之前经济评价是从探明储量上报开始,在勘探阶段对经济评价工作研究较少,缺乏一套适应当前油气勘探市场形势的经济评价理论和方法(郭元岭,2005)。海上油藏相较于陆上成本更高、风险更大,因此本文针对海上油藏勘探开发特点,利用现金流法建立计算模型,由于勘探阶段资料相对匮乏,本次主要通过数据统计和类比等方法,以最简化的方式  相似文献   

障壁坝砂体储层特征与成岩孔隙定量演化模式 ——以鄂尔多斯盆地延长探区本溪组为例   总被引：1，自引：1，他引：0  

胡鹏  于兴河  陈宏亮  赵晨帆  周进松  韩小琴  李亚龙 《沉积学报》2019,37(2):390-402

为明确海陆变迁背景下障壁坝砂体成岩孔隙演化规律,运用岩石薄片、扫描电镜及配套能谱、阴极发光等资料,对延长探区石炭系本溪组障壁成因砂体储集特征与成岩作用进行综合分析,并结合砂岩初始孔隙度恢复模型与薄片孔隙定量分析技术,开展基于埋藏热演化历程的储层孔隙演化参数定量评价,建立该区本溪组障壁坝砂岩孔隙定量演化模式。结果表明:储层砂岩以石英砂岩、岩屑质石英砂岩及岩屑砂岩为主;孔隙度、渗透率平均值分别为4.72%和1.22×10^(-3 )μm^2;储集空间以溶蚀扩大孔、粒内孔、晶间孔为主;现今储层主体已达到晚成岩阶段;砂岩初始孔隙度平均值为38.1%,埋藏至今共经历了四个典型的成岩增/减孔阶段,即P_1～T_2(285～208 Ma)"低地温、快埋藏"的大幅减孔阶段(-30.7%)、T_2～J_3(208～153 Ma)"高地温、缓沉降"的溶蚀增孔阶段(+3.9%)、J_3～K_1(153～96 Ma)"高地温、稳埋深"的减孔定型阶段(-6.6%)、K_1至今(96 Ma～)"低地温、晚隆升"的弱改造阶段。  相似文献   

松科二井邻域沙河子组含油气地层结构特征——基于测井和地震数据的分析          下载免费PDF全文

符伟  侯贺晟  张交东  刘财  冯晅  卢占武 《中国地质》2019,46(5):1052-1060

松辽盆地大陆深部科学钻探工程"松科二井"获得了最完整的沙河子组地层岩心,初步识别出深部页岩气气测异常43层,累计厚度102 m,显示出沙河子组地层具有良好的深部能源前景。为进一步分析松辽盆地沙河子组地层油气资源潜力,本文在前人研究的基础上,结合松科二井测井、岩心数据和地震数据,分析松科二井邻域沙河子组地层的层序特征和空间展布,同时以随钻录井记录到的气测异常为出发点,分析沙河子组地层的测井和地震响应。结果显示:松科二井邻域沙河子组地层具有厚度大、横向延续小的地层展布特点,根据测井、岩心及地震数据,将沙河子组地层分为4个三级层序:SQ1、SQ2、SQ3和SQ4,其中顶部SQ4层序具有较好的油气前景,其岩性以泥岩为主,并具有相对较高孔隙度、低波阻抗的测井曲线特征,在地震剖面上表现为连续强振幅,阻抗反演剖面上存在局部低波阻抗特征,揭示了该区沙河子组深层天然气资源的赋存条件。  相似文献