Special Solutions in a Simplified Restricted Three-Body Problem with Gravitational Radiation Taken into Account     

V. A. Brumberg 《Celestial Mechanics and Dynamical Astronomy》2003,85(3):269-291

The distinctive feature of the relativistic restricted three-body problem within the c ^–5 order of accuracy (2 post-Newtonian approximation) is the presence of the gravitational radiation. To simplify the problem the motion of the massive binary components is assumed to be quasi-circular. In terms of time these orbits have linearly changing radii and quadratically changing phase angles. By substituting this motion into the Newtonian-like equations of motion one gets the quasi-Newtonian restricted quasi-circular three-body problem sufficient to take into account the main indirect perturbations caused by the binary radiation terms. Such problem admits the Lagrange-like quasi-libration solutions and rather simple quasi-circular orbits lying at large distance from the binary.  相似文献   

安达曼弧与缅甸、云南强震相关性研究     

陈立德  付虹 《地震研究》2007,30(1):14-17

研究区包括安达曼弧、缅甸平原和云南地区三个部分。对安达曼弧7级以上地震与缅甸、云南7级和6.8级地震的群体与个体的相关特征进行了研究,发现安达曼弧、缅甸平原M≥7.0地震与云南M≥6.8地震在群体上有一定相关性,但并非一一相关。云南有4个地震活跃期,但安达曼弧与缅甸平原却只有3个,缺失第3活跃期。研究区强震活动从板缘向板内逐渐减弱,三个地区最大震级分别为8.7级、7.8级和7.7级。安达曼弧与缅甸、云南7级地震的个体相关概率分别为33%和27%,平均30%左右,缅甸与云南的个体相关概率为43%。最后对云南的地震趋势进行了预测。  相似文献   

Gamma-ray bursts: post-burst evolution of fireballs   总被引：3，自引：0，他引：3  

Y. F. Huang  Z. G. Dai  D. M. Wei  & T. Lu 《Monthly notices of the Royal Astronomical Society》1998,298(2):459-463

The post-burst evolution of fireballs that produce γ-ray bursts (GRBs) is studied, assuming the expansion of fireballs to be adiabatic and relativistic. Numerical results as well as an approximate analytic solution for the evolution are presented. Owing to the adoption of a new relation between t R and γ, our results differ markedly from previous studies. Synchrotron radiation from the shocked interstellar medium is carefully calculated, using a conventional set of equations. The observed X-ray flux of GRB afterglows can be reproduced easily. Although the optical afterglows seem much more complicated, our results can still present a rather satisfactory agreement with observations. We also find that the expansion will no longer be highly relativistic about 4 d after the main GRB. We thus suggest that the marginally relativistic phase of the expansion should be investigated so as to check the afterglows observed a week or more later.  相似文献   

Slim accretion discs: a model for ADAF–SLE transitions     

Igor V. Igumenshchev  Marek A. Abramowicz  & Igor D. Novikov 《Monthly notices of the Royal Astronomical Society》1998,298(4):1069-1078

We numerically construct slim, global, vertically integrated models of optically thin, transonic accretion discs around black holes, assuming a regularity condition at the sonic radius and boundary conditions at the outer radius of the disc and near the black hole. In agreement with several previous studies, we find two branches of shock-free solutions, in which the cooling is dominated either by advection or by local radiation. We also confirm that the part of the accretion flow where advection dominates is in some circumstances limited in size: it does not extend beyond a certain outer limiting radius. New results found in our paper concern the location of the limiting radius and the properties of the flow near to it. In particular, we find that beyond the limiting radius the advective-dominated solutions match on to Shapiro, Lightman &38; Eardley (SLE) discs through a smooth transition region. Therefore, the full global solutions are shock-free and unlimited in size. There is no need to postulate an extra physical effect (e.g. evaporation) for triggering the ADAF–SLE transition. It occurs as a result of standard accretion processes described by the classic slim disc equations.  相似文献   

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   

AMRVAC and relativistic hydrodynamic simulations for gamma-ray burst afterglow phases     

Zakaria Meliani  Rony Keppens  Fabien Casse  Dimitrios Giannios 《Monthly notices of the Royal Astronomical Society》2007,376(3):1189-1200

We apply a novel adaptive mesh refinement (AMR) code, AMRVAC (Adaptive Mesh Refinement version of the Versatile Advection Code), to numerically investigate the various evolutionary phases in the interaction of a relativistic shell with its surrounding cold interstellar medium (ISM). We do this for both 1D isotropic and full 2D jet-like fireball models. This is relevant for gamma-ray bursts (GRBs), and we demonstrate that, thanks to the AMR strategy, we resolve the internal structure of the shocked shell–ISM matter, which will leave its imprint on the GRB afterglow. We determine the deceleration from an initial Lorentz factor  γ= 100  up to the almost Newtonian     phase of the flow. We present axisymmetric 2D shell evolutions, with the 2D extent characterized by their initial opening angle. In such jet-like GRB models, we discuss the differences with the 1D isotropic GRB equivalents. These are mainly due to thermally induced sideways expansions of both the shocked shell and shocked ISM regions. We found that the propagating 2D ultrarelativistic shell does not accrete all the surrounding medium located within its initial opening angle. Part of this ISM matter gets pushed away laterally and forms a wide bow-shock configuration with swirling flow patterns trailing the thin shell. The resulting shell deceleration is quite different from that found in isotropic GRB models. As long as the lateral shell expansion is merely due to ballistic spreading of the shell, isotropic and 2D models agree perfectly. As thermally induced expansions eventually lead to significantly higher lateral speeds, the 2D shell interacts with comparably more ISM matter and decelerates earlier than its isotropic counterpart.  相似文献   

Equation of state in relativistic magnetohydrodynamics: variable versus constant adiabatic index     

A. Mignone  Jonathan C. McKinney 《Monthly notices of the Royal Astronomical Society》2007,378(3):1118-1130

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语言相对性与英语的区域性变体研究   总被引：1，自引：0，他引：1  

郭遂红 《广东海洋大学学报》2004,24(5):64-69

英语已发展成为一门世界性语言 ,英语在非英语国家的发展已经形成了许多带有浓厚地域特色的变体。从语言相对性的角度对英语区域性变体进行分析研究 ,论述其产生的历史根源是由于英国在世界上的扩张、以及文化差异 ,并阐述了英语区域性变体的分类以及人们对区域性变体所持的态度。  相似文献   

ISA accelerometer onboard the Mercury Planetary Orbiter: error budget     

Valerio Iafolla  David M. Lucchesi  Sergio Nozzoli  Francesco Santoli 《Celestial Mechanics and Dynamical Astronomy》2007,97(3):165-187

We have estimated a preliminary error budget for the Italian Spring Accelerometer (ISA) that will be allocated onboard the Mercury Planetary Orbiter (MPO) of the European Space Agency (ESA) space mission to Mercury named BepiColombo. The role of the accelerometer is to remove from the list of unknowns the non-gravitational accelerations that perturb the gravitational trajectory followed by the MPO in the strong radiation environment that characterises the orbit of Mercury around the Sun. Such a role is of fundamental importance in the context of the very ambitious goals of the Radio Science Experiments (RSE) of the BepiColombo mission. We have subdivided the errors on the accelerometer measurements into two main families: (i) the pseudo-sinusoidal errors and (ii) the random errors. The former are characterised by a periodic behaviour with the frequency of the satellite mean anomaly and its higher order harmonic components, i.e., they are deterministic errors. The latter are characterised by an unknown frequency distribution and we assumed for them a noise-like spectrum, i.e., they are stochastic errors. Among the pseudo-sinusoidal errors, the main contribution is due to the effects of the gravity gradients and the inertial forces, while among the random-like errors the main disturbing effect is due to the MPO centre-of-mass displacements produced by the onboard High Gain Antenna (HGA) movements and by the fuel consumption and sloshing. Very subtle to be considered are also the random errors produced by the MPO attitude corrections necessary to guarantee the nadir pointing of the spacecraft. We have therefore formulated the ISA error budget and the requirements for the satellite in order to guarantee an orbit reconstruction for the MPO spacecraft with an along-track accuracy of about 1 m over the orbital period of the satellite around Mercury in such a way to satisfy the RSE requirements.  相似文献   

The magnetohydrodynamics of stellar structures     

G. S. Dubey  U. S. Pandey  J. P. Singh  L. K. Singh  S. N. Singh 《Journal of Astrophysics and Astronomy》1990,11(1):23-28

The equation governing the equilibrium of a centrally-symmetric, self-gravitating distribution of matter is obtained by assuming that matter is described by magnetofluid and it is shown that the equation of stellar structure described by an ideal fluid is recovered when magnetic fieldh is vanishing  相似文献