A generalized nonideal magnetohydrodynamic (MHD) model to explore the excitation dynamics of the gravitational (Jeans) instability in a spherical complex molecular cloud is reported. It includes the realistic effects of viscoelasticity, buoyancy, polytropicity, volumetric expansion, and so forth. A standard technique of spherical normal mode analysis, without invoking any quasi-classic approximation over the non-Newtonian astrocloud, yields a unique type of generalized linear cubic dispersion relation. We see numerically that the equilibrium temperature and radial cloud size act as stabilizing (decelerating) agencies against the self-gravity. Contrariwise, the mean density and magnetic field act as destabilizing (accelerating) factors against the nonlocal cloud collapse. The various propagatory and phase-space features are illustrated. The magnetic field as a cloud destabilizer in spherical geometry to initialized astrostructure formation dynamics is a new result. Its source is in the concurrent action of the diversified meanfluidic non-ideality factors against the formal planar picture. It has interestingly a good agreement with the various earlier astronomic observations based on the experiments widely founded on the magneto-optic Zeeman effects.

中文翻译：

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具有几何曲率效应的非理想 MHD 等离子体云中的牛仔裤不稳定性


报道了一种广义非理想磁流体动力学 (MHD) 模型，用于探索球形复杂分子云中重力 (Jeans) 不稳定性的激发动力学。它包括粘弹性、浮力、多方性、体积膨胀等的真实效果。球面简正模分析的标准技术，无需对非牛顿星云进行任何准经典近似，即可产生一种独特类型的广义线性立方色散关系。我们从数字上看到，平衡温度和径向云大小充当对抗自重力的稳定（减速）机构。相反，平均密度和磁场充当非局域云塌陷的不稳定（加速）因素。说明了各种传播和相空间特征。磁场作为球面几何中的云不稳定因素来初始化天体结构形成动力学是一个新结果。其根源在于多样化的平均流体非理想因素对形式平面图像的同时作用。有趣的是，它与基于广泛建立在磁光塞曼效应的实验基础上的各种早期天文学观测结果有很好的一致性。