标题： 均匀拉长的密度分布。 二。 各向异性与旋转 显示英文标题

标题： Homeoidally striated density profiles. II. Anisotropy and rotation

摘要： 关于具有同心分层的雅可比椭球体，发展了一种系统旋转和特殊运动的统一理论，在这种理论中同时考虑了真实的和虚幻的旋转。 残余运动过量的正效应或负效应被证明分别等效于额外的真实或虚幻旋转。 然后发现，指定速度分布的具有同心分层的雅可比椭球体总是允许一个伴随构型，即与之质量相等且轴相同的经典雅可比椭球体。 此外，对于三轴配置，在主轴方向上的残余速度各向异性量上建立了进一步的约束条件。 特别致力于根据归一化参数研究引力平衡配置序列，包括密度和速度分布的影响。 特别是，显示了从轴对称到三轴配置的分支点出现的情况与经典的雅可比椭球体相同，这与早期的结果相反。 还解释了上述差异的原因。 以该模型为依据，对最近数值模拟有关稳定性结果的解释进行了提供。 从该模型的角度，简要回顾并讨论了早期哈勃序列的物理解释，如果椭圆星系被视为孤立系统或嵌入暗物质晕中。 无论如何，确定了扁平状配置的最小扁率。 另一方面，未发现拉长状配置的最小拉长量，而观测到的没有比E7更长的椭圆星系需要一种不同的物理解释，例如完全研究过的弯曲不稳定性。 显示英文摘要

摘要： With regard to homeoidally striated Jacobi ellipsoids, a unified theory of systematically rotating and peculiar motions is developed, where both real and imaginary rotation are considered. The effect of positive or negative residual motion excess, is shown to be equivalent to an additional real or imaginary rotation, respectively. Then it is realized that a homeoidally striated Jacobi ellipsoid with assigned velocity distribution, always admits an adjoint configuration i.e. a classical Jacobi ellipsoid of equal mass and axes. In addition, further constraints are established on the amount of residual velocity anisotropy along the principal axes, for triaxial configurations. Special effort is devoted to investigating sequences of virial equilibrium configurations in terms of normalized parameters, including the effects of both density and velocity profile. In particular, it is shown that bifurcation points from axisymmetric to triaxial configurations occur as in classical Jacobi ellipsoids, contrary to earlier results. The reasons of the above mentioned discrepancy are also explained. An interpretation of recent results from numerical simulations on stability (Meza 2002), is provided in the light of the model. A physical interpretation of the early Hubble sequence is shortly reviewed and discussed from the standpoint of the model, according if elliptical galaxies are considered as isolated systems or embedded within dark matter haloes. In any case, a lower limit to the flattening of oblate-like configurations is established. On the other hand, it is found no lower limit to the elongation of prolate-like configurations, and observed lack of elliptical galaxies more elongated than E7 needs a different physical interpretation, such as the fully investigated bending instabilities.