2011年3月7~8日永胜站震前舒曼谐振异常数值模拟分析

2011年3月10日中国云南盈江发生5.8级地震, 3月11日日本本州岛东海岸附近海域发生9.0级地震。 2011年3月7日、 8日云南永胜地磁台站观测到了舒曼谐振前4阶振幅异常增大。 本文建立了基于三维时域有限差分方法的舒曼谐振模型, 利用该模型对盈江地震对永胜站观测到的舒曼谐振影响进行了数值分析。 通过对实验和模拟结果进行分析, 认为此次云南永胜观测到的舒曼谐振异常不仅与日本地震相关也可能与云南盈江地震相关。     

极浅层稠油油藏油砂特征及潜力评价

油砂和浅层稠油是具有超低开发成本的两类非常规资源,非常规与历次油价下跌密切相关,使得这类资源成为了全球瞩目的焦点.春风油田兼具地表油砂和浅层稠油两类非常规,但岩心在地表会呈现极松散的不成型油砂,使得一些基础常规实验无法测定,影响到进一步分析评估.因此,需要针对这类非常规资源进行一系列新实验,即在常规实验的基础上,增加热物性、高温相渗、核磁共振等专项实验,并与常规实验结果进行比较.热物性实验发现,储层内部灰质、泥质夹层导热性良好,反映热波及效率会较高.相渗实验发现,油砂的油水相渗Kro和Krw的终点间距较大,两相覆盖范围宽,束缚水饱和度低,且孔隙越均匀,油相相对渗透率就越大.实验还发现,热物性、相渗、阵列感应实验得到的不同参数,相互之间存在一定相关性.利用新的核磁共振方法,可直接得到束缚水饱和度,获取原始含油饱和度,进而求取驱油效率,大大简化实验步骤和测试项目.最后,通过驱油效率计算和潜力评价发现,虽然经过多轮次吞吐,油砂目前的平均含油饱和度仍然很高,反映了稠油储量动用程度低,仍有很大的开发潜力.     

Modeling of Rapidly Rotating Thermal Convection Using Vorticity and Vector Potential

We have used a numerical scheme based on higher-order finite differences to investigate effects of adiabatic heating and viscous dissipation on 3-D rapidly rotating thermal convection in a Cartesian box with an aspect-ratio of 221. Although we omitted coupling with the magnetic field, which can play a key role in the dynamics of the Earth's core, the understanding of non-linear rotating convection including realistic thermodynamic effects is a necessary prerequisite for understanding the full complexity of the Earth's core dynamics. The system of coupled partial differential equations has been solved in terms of the principal variables vorticity , vector potential A and temperature T. The use of the vector potential A allows the velocity field to be calculated with one spatial differentiation in contrast to the spheroidal and toroidal function approach. The temporal evolution is governed by a coupled time-dependent system consisting of and T. The equations are discretized in all directions by using an eighth-order, variable spaced scheme. Rayleigh number Ra of 10⁶, Taylor number Ta of 10⁸ and a Prandtl number Pr of 1 have been employed. The dissipation number of the outer core was taken to be 0.2. A stretched grid has been employed in the vertical direction for resolving the thin shear boundary layers at the top and bottom. This vertical resolution corresponds to around 240 regularly spaced points with an eighth-order accuracy. For the regime appropriate to the Earth's outer core, the dimensionless surface temperature T ₀ takes a large value, around 4. This large value in the adiabatic heating/cooling term is found to cause stabilization of both the temperature and velocity fields.     

A Symplectic Mapping Model for the Study of 2:3 Resonant Trans-Neptunian Motion

A symplectic mapping is constructed for the study of the dynamical evolution of Edgeworth-Kuiper belt objects near the 2:3 mean motion resonance with Neptune. The mapping is six-dimensional and is a good model for the Poincaré map of the real system, that is, the spatial elliptic restricted three-body problem at the 2:3 resonance, with the Sun and Neptune as primaries. The mapping model is based on the averaged Hamiltonian, corrected by a semianalytic method so that it has the basic topological properties of the phase space of the real system both qualitatively and quantitatively. We start with two dimensional motion and then we extend it to three dimensions. Both chaotic and regular motion is observed, depending on the objects' initial inclination and phase. For zero inclination, objects that are phase-protected from close encounters with Neptune show ordered motion even at eccentricities as large as 0.4 and despite being Neptune-crossers. On the other hand, not-phase-protected objects with eccentricities greater than 0.15 follow chaotic motion that leads to sudden jumps in their eccentricity and are removed from the 2:3 resonance, thus becoming short period comets. As inclination increases, chaotic motion becomes more widespread, but phase-protection still exists and, as a result, stable motion appears for eccentricities up to e = 0.3 and inclinations as high as i = 15°, a region where plutinos exist.     

Chaotic transitions in resonant asteroidal dynamics

The utilization of chaotic dynamics approaches allowed the identification of many modes of motion in resonant asteroidal dynamics. As these dynamical systems are not integrable, the motion modes are not separated and one orbit may transit from one mode to another. In some cases, as in the \31 resonance, these transitions may lead, in a relatively short time scale, to eccentricities so high that the asteroid may approach the Sun and be destroyed. In the \21 and \32 resonances these transitions are much slower and only indirect estimations of the time which is needed for a generic asteroid to leave the resonance are possible. It may reach hundreds of million years in the more robust regions of the \21 resonance and a time of the order of billions of years in those of the \32 resonance. These values are consistent with the observed depletion of the \21 resonance (only a few asteroids known while almost 60 asteroids are known in the \32 resonance).     

Critical point families at the 3:1 resonance

An enlarged averaged Hamiltonian is introduced to compute some families of periodic orbits of the planar elliptic 3-body problem, in the Sun-Jupiter-Asteroid system, near the 3:1 resonance. Five resonant families are found and their stability is studied, The families of symmetric periodic orbits of the elliptic problem appear near the corresponding fixed points which have been computed in this model and the coincidence is good for moderate values of the eccentricity of the asteroid for two of these families; the other three families do not fulfil the Sundman condition and they cannot be considered as families of periodic orbits of the real model.     

Numerical investigation on the orbital evolution of 1:2 resonant asteroids between Jupiter and Saturn

According to some investigations (Lecar and Franklin, 1973; Franklin et al., 1989; Soper et al., 1990) asteroids cannot remain for along time between Jupiter and Saturn. But as it is well known there is a near 5:2 commensurability between Jupiter and Saturn. So there might be a possibility that asteroids between Jupiter and Saturn could be trapped in a resonant relation.In order to investigate this possibility, the changes of orbital elements of an asteroid whose initial value of semi-major axis corresponds to that of a 1:2 resonant orbit were investigated by means of a double precision Cowell method. The integration routine was kindly supplied by Dr Yoshikawa.We considered first a planar restricted problem of three bodies, Sun-Jupiter-Asteroid, then a four body problem, Sun-Jupiter-Asteroid-Saturn. When integrating the equations of motion, short periodic terms were not eliminated and in the second test the interactions between Jupiter and Saturn were retained. Whether a close approach occured or not was not investigated. In every case a _j = 5.20, a _s = 9.54 and a = 8.26 were adopted as initial values of the semi-major axis of Jupiter, Saturn and Asteroid respectively.     

On The Effect of Short-Period Terms in Resonance Trapping

In this paper we study the effects of short-period perturbations in the planar asteroidal problem with Stokes drag. The averaging of the dissipative terms is extended to show the appearance of crossed-terms which, in most commensurabilities, are more important than several zeroth-order terms calculated in previous works. In the case of resonance trapping in a libration point, we also discuss the effects of the eccentricity of the perturber in the stationary solution. For the so-called ‘universal eccentricity’, we show that the contributions due to both, short-period terms and harmonics of the auxiliary resonant angle, lead to a corrected value which is no longer invariant. The most significant dependence of this new librational eccentricity is with the eccentricity of the perturber, although a slight variation is also noted with respect to the chosen drag coefficient. In all cases, we present comparisons with numerical simulations of the exact N-body equations. This revised version was published online in July 2006 with corrections to the Cover Date.     

Higher order resonant orbits

I present higher-order resonances of the tube and boomerang orbits in the co-rotating meridional plane of an axisymmetric galactic potential. Additionally, mirror forms of these orbits are given.     

Estimating Mercury's 88-day libration amplitude from orbit

In this paper it is derived that the libration of Mercury can be described by where Φ₀ is the unknown libration amplitude, M is Mercury's mean anomaly and K=−9.483. Φ₀ can be determined by comparing pairs of images of the same landmarks taken by an orbiter at different positions of Mercury. If the angle between the orbit plane of a polar orbiter and Mercury's line of periapsis is between −60° and 60° and if one landmark at the equator is imaged per day with a relative precision of , then the libration amplitude can be determined in two Mercury years (176 days) with an accuracy of or better, which is sufficient to answer the question whether Mercury has a solid or fluid core.