对 Hamilton 等人《为什么银河系盘面如此冷？》一文的评论
A comment on "Why is the Galactic disk so cool?", by Hamilton et al
AI总结：
本文指出，我们2002年提出并经3D运动修正的径向迁移模型能自然解释Frankel等人关于银河系盘面恒星角动量扩散快于加热的发现，表明无需修改旋臂结构理论，且排除了其他加热机制的余地。
摘要：
Frankel 等人（2020）报告称，银河系盘面中恒星角动量扩散的速率大约比加热速率快十倍，这对盘面恒星散射的性质提出了严格要求。在最近的一篇贴文中，Hamilton 等人（2024）在包含瞬时旋臂的银河系模型中积分了测试粒子的轨道，并发现他们计算中加热速率与径向迁移速率的比值通常大于 Frankel 等人报告的值。他们得出结论，观测到的缓慢加热速率对银河系动力学模型构成了重大挑战，似乎需要修改我们当前的旋臂结构理论。在此我们表明，我们于 2002 年发表并在经过 3D 运动修正后的径向迁移模型，能够自然地解释 Frankel 等人的发现，但几乎没有给瞬时旋臂以外的其他机制造成的额外加热留下空间。
英文摘要：
Frankel et al (2020) reported that the rate of diffusion in angular momentum by stars in the disk of the Milky Way was about ten times faster than the rate of heating, which places a stringent requirement on the nature of disk star scattering. In a recent posting, Hamilton et al (2024) integrated orbits of test particles in a Galactic model that included transient spirals, and found that the ratio of the rates heating to radial migration in their calculations was generally larger than reported by Frankel et al. They concluded that the observed slow heating rate poses a significant challenge to dynamical models of the Milky Way and seemed to require revision of our current theories of spiral structure. Here we show that that our earlier models of radial migration we published in 2002, after correction for 3D motion, account naturally for the finding of Frankel et al, but leave little room for additional heating by mechanisms other than transient spirals.
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