对恒星中捕获的暗物质粒子速度分布的不确定性的更严格处理
Towards a more rigorous treatment of uncertainties on the velocity distribution of dark matter particles for capture in stars
摘要：
恒星中的暗物质（DM）捕获提供了丰富的现象学，使得在不同的天体物理环境中探测各种各样的粒子DM场景成为可能。尽管几十年来的改进，以完善捕获相关的观测值的预测和更好地量化天体物理和粒子物理的不确定性，银河系相空间分布函数DM的实际影响被忽视了。在这项工作中，我们解决这个问题，利用自洽平衡相空间模型的基础上爱丁顿反演形式主义和扩展这种方法的DM晕在速度空间中具有一定程度的各向异性。我们证明，不正确的占DM速度分布与银河系中的位置的变化导致一个系统误差之间的一个因素，两个数量级，特别是取决于目标恒星，DM候选人的质量和类型的相互作用。此外，我们表明，潜在的相空间属性，如速度张量的各向异性，实际上发挥了重要的作用-以前被忽视-可以有相当大的影响预测捕获率和随后的观测。我们认为，爱丁顿的方法，自洽占银河系的组成部分的运动学约束，实际上提供了一个可靠的下一个最小的方法来缩小不确定性相空间模型的预测DM捕获相关的可观测量在恒星。
英文摘要：
Dark matter (DM) capture in stars offers a rich phenomenology that makes it possible to probe a wide variety of particle DM scenarios in diverse astrophysical environments. In spite of decades of improvements to refine predictions of capture-related observables and better quantify astrophysical and particle-physics uncertainties, the actual impact of the Galactic phase-space distribution function of DM has been overlooked. In this work, we tackle this problem by making use of self-consistent equilibrium phase-space models based on the Eddington inversion formalism and an extension of this method to a DM halo with some degree of anisotropy in velocity space. We demonstrate that incorrectly accounting for the variation of the DM velocity distribution with position in the Galaxy leads to a systematic error between a factor two and two orders of magnitude, depending in particular on the target star, the DM candidate mass and the type of interaction involved. Moreover, we show that underlying phase-space properties, such as the anisotropy of the velocity tensor, actually play an important part -- previously disregarded -- and can have a sizable impact on predictions of capture rates and subsequent observables. We argue that Eddington-like methods, which self-consistently account for kinematic constraints on the components of the Galaxy, actually provide a reliable next-to-minimal approach to narrow down uncertainties from phase-space modeling on predictions of observables related to DM capture in stars.
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