kappa修正极化力对非热EiBI引力尘埃云中Jeans不稳定性的影响
Effect of kappa-modified polarization force on Jeans instability in nonthermal EiBI-gravitating dust clouds
AI总结：
本文开发半解析模型研究kappa分布较轻组分及kappa修正极化力对尘埃分子云中Jeans不稳定性的影响，发现kappa修正极化力和负EiBI引力参数具有不稳定化作用，为致密DMCs超紧凑HII区域小天体结构形成提供新见解。
摘要：
本文开发了一个半解析模型，以研究kappa分布的较轻组分及其相关的kappa修正极化力对尘埃分子云（DMCs）中经典Jeans不稳定性的影响。组成电子和离子被认为遵循非热kappa速度分布定律，而组成的大质量尘埃颗粒被视为EiBI引力流体。利用球面简正模分析推导出了线性化的二次色散关系。在流体动力学和动力学状态下分析了所得的色散关系及其相应的修正不稳定性判据。对振荡和传播模式的特征进行了图示分析。结果表明，EiBI引力在色散关系中引入了一个新的速度项。相比之下，非热kappa分布的组分显著增强了极化力，超过了它们各自的Maxwellian对应物。与正EiBI参数不同，kappa修正极化力和负EiBI引力参数具有不稳定化影响。增强的极化相互作用参数和正EiBI参数降低了实归一化频率。因此，相速度表现出强烈的色散，随波数增加直至达到饱和，之后过渡到弱色散状态。这些发现为通过致密DMCs超紧凑HII区域的非局域Jeans不稳定性形成更小天体结构提供了新见解。
英文摘要：
A semi-analytic model is developed to study the effects of kappa-distributed lighter constituents and the associated kappa-modified polarization force on the classical Jeans instability in dust molecular clouds (DMCs). The constitutive electrons and ions are considered to follow a nonthermal kappa-velocity distribution law, while the constitutive massive dust grains are treated as the EiBI-gravitating fluids. A linearized quadratic dispersion relation is derived using spherical normal mode analysis. The resulting dispersion relation and its corresponding modified instability criteria are analyzed in the hydrodynamic and kinetic regimes. The oscillatory and propagating mode characteristics are illustratively analyzed. It is seen that the EiBI gravity introduces a new velocity term in the dispersion relation. In contrast, the nonthermal kappa-distributed constituents significantly enhance the polarization force against their respective Maxwellian counterparts. The kappa-modified polarization force and the negative EiBI gravity parameter have destabilizing influences, unlike the positive EiBI parameter. An enhanced polarization interaction parameter and a positive EiBI parameter reduce the real normalized frequency. Consequently, the phase velocity exhibits strong dispersion, increasing with wavenumber until reaching saturation, after which it transitions into a weakly dispersive regime. These findings provide new insights into the formation of smaller astrophysical structures via the non-local Jeans instability in the ultracompact HII regions of dense DMCs.
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