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大别山北部饶拔寨超镁铁岩体微量元素地球化学 总被引：3，自引：4，他引：3
本文报道了饶拔寨超镁铁岩体的5个钻孔15个岩心样品的主量元素和微量元素成分。该岩体由上、下两部分构成。岩性以方辉橄榄岩为主，纯橄榄岩和二辉橄榄岩次之。主量元素成分表明岩体由饱满地幔经过不同程度部分熔融，形成了亏损程度不同的大陆岩石圈地幔。总体上下部岩体较上部亏损程度大。原始地幔标准化REE等不相容微量元素丰度模式表明岩体在熔融作用后又经过了地幔交代作用，形成不同程度LREE和LILE的富集。样品中有角闪石和金云母等含水矿物，表明有实性地幔交代作用。对比LREE与LILE的富集特征，表明可能有两类地幔交代作用，有两种不同性质的交代介质，LREE和Sr等的富集可能与硅酸盐熔体有关，而Rb、Ba、K等的富集可能与俯冲带流体活动有关。总体上下部岩体的交代作用较上部岩体的强。 相似文献
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Incontrovertible evidence is presented that the force-free magnetic fields exhibit strong stochastic behavior. Arnold's solution is given with the associated first integral of energy. A subset of the solution is shown to be non-ergodic whereas the full solution is shown to be ergodic. The first integral of energy is applied to the study of these fields to prove that the equilibrium points of such magnetic configurations are saddle points. Finally, the potential function of the first integral of energy is shown to be a member of the Helmholtz family of solutions. Numerical results corroborate the theoretical conclusions and demonstrate the robustness of the energy integral, which remains constant for arbitrarily long computing times. 相似文献
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G. J. J. Botha F. H. Busse N. E. Hurlburt A. M. Rucklidge 《Monthly notices of the Royal Astronomical Society》2008,387(4):1445-1462
A numerical model of axisymmetric convection in the presence of a vertical magnetic flux bundle and rotation about the axis is presented. The model contains a compressible plasma described by the non-linear MHD equations, with density and temperature gradients simulating the upper layer of the Sun's convection zone. The solutions exhibit a central magnetic flux tube in a cylindrical numerical domain, with convection cells forming collar flows around the tube. When the numerical domain is rotated with a constant angular velocity, the plasma forms a Rankine vortex, with the plasma rotating as a rigid body where the magnetic field is strong, as in the flux tube, while experiencing sheared azimuthal flow in the surrounding convection cells, forming a free vortex. As a result, the azimuthal velocity component has its maximum value close to the outer edge of the flux tube. The azimuthal flow inside the magnetic flux tube and the vortex flow is prograde relative to the rotating cylindrical reference frame. A retrograde flow appears at the outer wall. The most significant convection cell outside the flux tube is the location for the maximum value of the azimuthal magnetic field component. The azimuthal flow and magnetic structure are not generated spontaneously, but decay exponentially in the absence of any imposed rotation of the cylindrical domain. 相似文献