根据Lambda CDM N体模拟结果计算反物质宇宙射线的团簇增强因子
Full calculation of clumpiness boost factors for antimatter cosmic rays in the light of Lambda-CDM N-body simulation results
摘要：
反质子和正电子银河宇宙线谱是间接探测暗物质的关键目标之一。增强因子，对应于信号的增强，并与暗物质分布的聚集特性有关，在过去已经被认为高达数千。这些助推因子对于反粒子的间接探测的巨大影响，例如PAMELA卫星或即将到来的AMS-02实验，要求对其进行详细的计算。我们考虑到高分辨率N体暗物质模拟的结果，计算最有可能的能量相关的助推因子与宇宙射线的传播特性，反质子和正电子。从次晕的质量分布和空间分布出发，利用反质子和正电子传播子计算了次晕初级通量增强因子的平均值和方差。我们利用Lavalle等人（2007）中介绍的统计方法，并与Monte Carlo计算结果进行交叉检查。通过跨越一些极端的配置的子晕和传播特性，我们发现，平均贡献的团块是可以忽略不计相比，光滑的暗物质组件。子晕不会导致信号的增强，除非它们具有某些极端（意想不到）的特性。这一结果是独立的性质的自湮灭暗物质候选人考虑，并提供精确的估计的理论和统计不确定性的反物质通量从暗物质子结构。在反物质通量测量中仍然可以预期光谱失真，但是我们的分析强烈反对调用大的甚至是轻微的团块增强因子的情况。
英文摘要：
Anti-proton and positron Galactic cosmic ray spectra are among the key targets for indirect detection of dark matter. The boost factors, corresponding to an enhancement of the signal and linked to the clumpiness properties of the dark matter distribution, have been taken as high as thousands in the past. The dramatic impact of these boost factors for indirect detection of antiparticles, for instance with the PAMELA satellite or the coming AMS-02 experiment, asks for their detailed calculation. We take into account the results of high resolution N-body dark matter simulations to calculate the most likely energy dependent boost factors linked to the cosmic ray propagation properties, for anti-protons and positrons. Starting from the mass and space distributions of sub-halos, the anti-proton and positron propagators are used to calculate the mean value and the variance of the boost factor for the primary fluxes. We take advantage of the statistical method introduced in Lavalle et al. (2007) and cross-check the results with Monte Carlo computations. By spanning some extreme configurations of sub-halo and propagation properties, we find that the average contribution of the clumps is negligible compared to that of the smooth dark matter component. Sub-halos do not lead to enhancement of the signals, unless they are taken with some extreme (unexpected) properties. This result is independent of the nature of the self-annihilating dark matter candidate considered, and provides precise estimates of the theoretical and the statistical uncertainties of the antimatter flux from dark matter substructures. Spectral distortions can still be expected in antimatter flux measurements, but scenarios invoking large and even mild clumpiness boost factors are strongly disfavoured by our analysis.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
