春晓气田泥岩垮塌测井数据校正及应用     

谢月芳  陈敏 《海洋地质译丛》2009,(4):73-76

由于存在部分泥岩井眼垮塌，东海春晓气田测井曲线砂泥岩阻抗部分叠置。针对这一现象，采用未垮塌段泥岩伽马与密度拟合关系校正垮塌段泥岩密度，声波时差经本区伽德那公式拟合后求取。通过泥岩垮塌测井数据校正前后对比、直方交会、岩石物理、正演及反演效果分析，认为校正后的测井数据比较真实地反映垮塌段扩径泥岩地层特征，储层与围岩波阻抗差异明显，为储层反演、砂体空间展布分析提供了有力依据。  相似文献   

Multidimensional treatment of photon emission from accretion discs around black holes     

Kazunori Kohri  Ken Ohsuga  Ramesh Narayan 《Monthly notices of the Royal Astronomical Society》2007,381(3):1267-1274

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A toy model for magnetic connection in black hole accretion disc     

Ding-Xiong Wang  Yong-Chun Ye  Yang Li  Dong-Mei Liu 《Monthly notices of the Royal Astronomical Society》2007,374(2):647-656

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New flaring of an ultraluminous X-ray source in NGC 1365     

R. Soria  A. Baldi  G. Risaliti  G. Fabbiano  A. King  V. La Parola  A. Zezas 《Monthly notices of the Royal Astronomical Society》2007,379(4):1313-1324

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Resonant relaxation near a massive black hole: the dependence on eccentricity     

M. Atakan Gürkan  Clovis Hopman 《Monthly notices of the Royal Astronomical Society》2007,379(3):1083-1088

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

T. Okuda  V. Teresi  D. Molteni 《Monthly notices of the Royal Astronomical Society》2007,377(4):1431-1438

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.  相似文献   

黑洞吸积理论及其天体物理学应用的近期发展(Ⅱ)   总被引：1，自引：0，他引：1  

袁峰 《天文学进展》2007,25(4):285-295

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.  相似文献   

加蓬G4-188区块钻井技术实践认识     

石强 《海洋地质译丛》2008,(1):82-87

加蓬G4-188区块是一个新的海外勘探区块,在钻井过程中遇到了井壁垮塌、气侵、井斜控制困难等诸多难题,影响了钻井施工的速度。针对这些难题,实施了解决G4-188区块钻井施工难点的各项技术措施,为G4-188区块后续钻井施工提供了有益的技术支持。  相似文献   

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

Sheng-Miao Wu  Ting-Gui Wang 《Monthly notices of the Royal Astronomical Society》2007,378(3):841-851

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.  相似文献   

Disc–jet coupling in black hole accretion systems – I. General relativistic magnetohydrodynamical models     

Jonathan C. McKinney  Ramesh Narayan 《Monthly notices of the Royal Astronomical Society》2007,375(2):513-530

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