Non-axisymmetric relativistic Bondi–Hoyle accretion on to a Schwarzschild black hole     

José A. Font  & J. M. Ibáñez 《Monthly notices of the Royal Astronomical Society》1998,298(3):835-846

We present the results of an exhaustive numerical study of fully relativistic non-axisymmetric Bondi–Hoyle accretion on to a moving Schwarzschild black hole. We have solved the equations of general relativistic hydrodynamics with a high-resolution shock-capturing numerical scheme based on a linearized Riemann solver. The numerical code was previously used to study axisymmetric flow configurations past a Schwarzschild black hole. We have analysed and discussed the flow morphology for a sample of asymptotically high Mach number models. The results of this work reveal that initially asymptotic uniform flows always accrete on to the hole in a stationary way, which closely resembles the previous axisymmetric patterns. This is in contrast with some Newtonian numerical studies where violent flip-flop instabilities were found. As discussed in the text, the reason can be found in the initial conditions used in the relativistic regime, as they cannot exactly duplicate the previous Newtonian setups where the instability appeared. The dependence of the final solution on the inner boundary condition as well as on the grid resolution has also been studied. Finally, we have computed the accretion rates of mass and linear and angular momentum.  相似文献   

Resonant tidal disruption in galactic nuclei     

Kevin P. Rauch  & Brian Ingalls 《Monthly notices of the Royal Astronomical Society》1998,299(4):1231-1241

It has recently been shown by Rauch 38 Tremaine that the rate of angular momentum relaxation in nearly Keplerian star clusters is greatly increased by a process termed 'resonant relaxation'; it was also argued, via a series of scaling arguments, that tidal disruption of stars in galactic nuclei containing massive black holes could be noticeably enhanced by this process. We describe here the results of numerical simulations of resonant tidal disruption which quantitatively test the predictions made by Rauch 38 Tremaine. The simulation method is based on an N -body routine incorporating cloning of stars near the loss cone and a semirelativistic symplectic integration scheme. Normalized disruption rates for resonant and non-resonant nuclei are derived at orbital energies both above and below the critical energy, and the corresponding angular momentum distribution functions are found. The black hole mass above which resonant tidal disruption is quenched by relativistic precession is determined. We also briefly describe the discovery of chaos in the Wisdom–Holman symplectic integrator applied to highly eccentric orbits and propose a modified integration scheme that remains robust under these conditions. We find that resonant disruption rates exceed their non-resonant counterparts by an amount consistent with the predictions; in particular, we estimate the net tidal disruption rate for a fully resonant cluster to be about twice that of its non-resonant counterpart. No significant enhancement in rates is observed outside the critical radius. Relativistic quenching of the effect is found to occur for hole masses M  >  M _Q  = (8 ± 3) × 10⁷  M . The numerical results combined with the observed properties of galactic nuclei indicate that for most galaxies the resonant enhancement to tidal disruption rates will be very small.  相似文献   

Radiatively driven mass accretion on to galactic nuclei by circumnuclear starbursts     

Masayuki Umemura  Jun Fukue  & Shin Mineshige 《Monthly notices of the Royal Astronomical Society》1998,299(4):1123-1131

We examine the physical processes of radiatively driven mass accretion on to galactic nuclei, owing to intensive radiation from circumnuclear starbursts. The radiation from a starburst not only causes the inner gas disc to contract via radition flux force, but also extracts angular momentum owing to relativistic radiation drag, thereby inducing an avalanche of the surface layer of the disc. To analyse such a mechanism, the radiation–hydrodynamical equations are solved, including the effects of the radiation drag force as well as the radiation flux force. As a result, it is found that the mass accretion rate owing to the radiative avalanche is given by M ˙ ( r )= η ( L _*/ c ²)( r / R )² (Δ R / R )(1 −  e ^−τ) at radius r , where the efficiency η ranges from 0.2 up to 1, L _* and R are respectively the bolometric luminosity and the radius of the starburst ring, Δ R is the extent of the emission regions, and τ is the face-on optical depth of the disc. In an optically thick regime, the rate depends upon neither the optical depth nor the surface mass density distribution of the disc. The present radiatively driven mass accretion may provide a physical mechanism which enables mass accretion from 100-pc scales down to ∼ parsec scales, and it may eventually be linked to advection-dominated viscous accretion on to a massive black hole. The radiation–hydrodynamical and self-gravitational instabilities of the disc are briefly discussed. In particular, the radiative acceleration possibly builds up a dusty wall, which 'shades' the nucleus in edge-on views. This provides another version of the model for the formation of an obscuring torus.  相似文献   

GPS和GLONASS系统下RAIM空洞预报     

任锴  杨力 《全球定位系统》2009,34(4):25-28,36

接收机自主完好性监测（RAIM）是卫星导航系统完好性监测的方法之一。一定时空条件下的RAIM可用性，可以通过RAIM空洞直观的反映出来，可以为飞行提供预警；利用不同期GPS、GLONASS实际星座，仿真分析了单星座以及GPS／GLONASS组合星座RAIM可用性，绘制了RAIM空洞图，具有一定的参考价值。  相似文献   

Evidence of the Link between Broad Emission Line Regions and Accretion Disks in Active Galactic Nuclei     

Yun Xu    Xin-Wu Cao Shanghai Astronomical Observatory  Chinese Academy of Sciences  Shanghai  Graduate School of Chinese Academy of Sciences  Beijing 《中国天文和天体物理学报》2007,7(1):63-70

1 INTRODUCTION Most bright active galactic nuclei (AGNs) exhibit broad emission lines, with full width at half maximum (FWHM ≥ 103 km s?1) (Peterson et al. 1999). Some type 1 AGNs could have very broad emission lines (FWHM≥ 20 000 km s?1). Type 2 AGNs s…  相似文献   

Evolution of the angular momentum of primordial black holes in a hot universe     

G. S. Bisnovatyi-Kogan  O. Yu. Tsupko 《Astrophysics》2007,50(4):544-547

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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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张为民  王勇 《大地测量与地球动力学》2007,27(4):44-46

??10???????FG5-112?????????????й???????????????????о?????嶯??????????????????????68??????????ι????????????С??2??10 ^-8 ms ^-2???????????????????????С?????????????;????????????????????????????????????仯?????1??10 ^-8 ms ^-2 /a??????????λ???????-0.38 cm/a;??????????λ?仯??????????????????????????????  相似文献   

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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