局域椭圆星系作为强弛豫、无碰撞、无耗散系统的密度分布
The Density Profile of Local Ellipticals as Violently Relaxed, Collisionless, Dissipationless Systems
摘要：
在最近的一系列论文中，一种新的形式主义已经发展起来，它解释了暗物质晕的内部结构，即通过合并和吸积以典型的宇宙学速率组装的无碰撞、无耗散系统。附近的椭圆星系也是无碰撞、无耗散的系统，通过合并聚集它们的质量，但与以前的结构相反，它们不连续地吸积外部物质，因为它们被宿主晕屏蔽。在这里，我们探讨的想法，他们自己的物质喷射的光环内的一个暴力合并之际，可以发挥类似的作用，外部吸积晕。预测的恒星质量密度分布与观测值吻合较好，并恢复了经验的总质量密度分布。
英文摘要：
In a series of recent papers, a new formalism has been developed that explains the inner structure of dark matter halos as collisionless, dissipationless systems assembled through mergers and accretion at the typical cosmological rate. Nearby ellipticals are also collisionless, dissipationless systems assembling their mass through mergers, but contrarily to the former structures they do not continuously accrete external matter because they are shielded by their host halos. Here we explore the idea that the infall of their own matter ejected within the halo on the occasion of a violent merger can play a role similar to external accretion in halos. The predicted stellar mass density profile fits the observed one, and the empirical total mass density profile is also recovered.
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