星系壳层前身天体中的能量演化：一个半解析模型
Energy evolution in the progenitor of galaxy shells: a semi-analytical model
AI总结：
本文提出一个半解析模型，研究矮星系前身在并合瓦解过程中粒子能量和角动量的变化，揭示自引力对壳层形成的关键作用，并证明精确建模前身能量范围对预测可观测壳层数量至关重要。
摘要：
围绕椭圆星系的恒星壳层是并合过程中被瓦解的矮星系遗迹，它们揭示了前身矮星系的能量和角动量分布。我们建立了一个半解析模型，用于描述粒子在首次内落过程中能量$ΔE_i$和角动量$ΔLz_i$的变化。我们表明，这些由前身天体自引力引起的变化对于展宽Plummer或Hernquist前身模型的初始能量分布具有重要作用。因此，这些变化对壳层的形成至关重要。在前身天体势瓦解之后的自由下落阶段，粒子不再受自引力束缚，而是在目标星系的引力势中运动。我们研究了做径向运动的粒子的径向周期与能量之间的关系。我们表明，对瓦解时矮星系能量范围的精确建模对于预测可观测壳层的数量是必不可少的。
英文摘要：
The stellar shells surrounding an elliptical galaxy, as remnants of a dwarf galaxy disrupted during merging, reveal the distribution of energy and angular momentum of the progenitor dwarf galaxy. We develop a semi-analytical model to describe the changes of energy $ΔE_i$ and angular momentum $ΔLz_i$ for particles during the first infall. We show that these changes, induced by the self-gravity of the progenitor, are important in broadening the initial energy distribution of the Plummer or Hernquist progenitor model. Consequently, these changes are crucial in shaping the shells. In the free fall stage following the disintegration of the progenitor potential, particles are no longer bound by self-gravity but move within the gravitational potential of the target galaxy. We investigate the relationship between the radial period and the energy of particles undergoing radial motion. We show that an accurate model of the energy range of the dwarf galaxy at disruption is essential to predict the number of observable shells.
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