标题： 振荡星震学对暗物质相互作用的限制和暗示 显示英文标题

标题： Asteroseismological constraints on--and hints of--dark matter interactions

摘要： 如果暗物质与原子核或电子相互作用，则与恒星组成部分的弹性碰撞会导致一些银河系暗物质的速度低于逃逸速度并变得引力束缚。 对于不对称暗物质（不会自湮灭），大量累积的暗物质可以作为额外的热传输源，改变恒星结构和演化。 这些效应可以通过恒星振荡学来探测。 在这里，我们通过数值模拟演示了这种效应。 我们使用蒙特卡洛校准的热传输计算，重点关注略大于太阳质量的恒星对流核心的消失。 我们利用一颗附近亚巨星的恒星振荡学数据，得出了自旋依赖的暗物质-核子和暗物质-电子相互作用的限制。 更引人注目的是，我们发现对于暗物质质量为$\gtrsim 4 \sigma$GeV 和截面为$\lesssim 3.5$cm$\sigma_{\chi-e} \sim 10^{-34.5}$的暗物质-电子相互作用存在$^2$偏好，尽管这与基于地球的直接探测实验的结果有强烈的冲突。 显示英文摘要

摘要： If dark matter interacts with nuclei or electrons, then elastic collisions with constituents of stars will cause some of the galactic dark matter to fall below the escape velocity and become gravitationally bound. For asymmetric dark matter (which does not self-annihilate), the large accumulated population of dark matter can act as an additional source of heat transport, altering stellar structure and evolution. These effects can be probed by the use of asteroseismology. Here, we demonstrate this effect via numerical simulations. We use Monte Carlo-calibrated heat transport calculations, with a focus on the erasure of the convective core in stars that are slightly more massive than the Sun. We find limits on spin-dependent dark matter-nucleon and dark matter-electron interactions using asteroseismological data from a nearby sub-giant star. More tantalizingly, we find a $\gtrsim 4 \sigma$ preference for dark matter-electron interactions for dark matter masses $\lesssim 3.5$ GeV and cross sections $\sigma_{\chi-e} \sim 10^{-34.5}$ cm$^2$, albeit in strong tension with limits from Earth-based direct detection experiments.