用脉冲星计时的康普顿和德布罗意尺度调制识别轴对称暗物质
Recognising Axionic Dark Matter by Compton and de-Broglie Scale Modulation of Pulsar Timing
摘要：
在弦论的推动下，轻轴子暗物质越来越受到“无WIMP时代”的青睐。星系形成被抑制低于金斯尺度，$\simeq 10^8 M_\odot$的轴子质量设置为，$m_B \sim 10^{-22}$ eV，和矮星系的大暗核的德布罗意尺度上的孤子解释。这是有说服力的，但在康普顿频率$ω_B= (2.5{\rm \, months})^{-1}(m_B/10^{-22}eV)$的固有标量场振荡的检测将是决定性的。通过演化玻色-爱因斯坦凝聚体的耦合薛定谔-泊松方程，我们预测暗物质完全受到德布罗意干涉的调制，在银河系中心有一个尺寸为$\simeq 150pc$的致密孤子核。振荡的场压导致广义相对论时间膨胀，与当地的暗物质密度成比例，在这个致密的核心内的暗物质具有可检测到的大的定时残差，即$\simeq 400nsec/(m_B/10^{-22}eV)$。这是令人鼓舞的，因为在银河系中心附近应该会发现许多新的行星，并计划进行无线电调查。更一般地说，在整个银河系中，两对星系星之间的暗物质密度差异会留下一个两两的银心特征，可以从各向同性的引力波背景中区分出来。
英文摘要：
Light Axionic Dark Matter, motivated by string theory, is increasingly favored for the "no-WIMP era". Galaxy formation is suppressed below a Jeans scale, of $\simeq 10^8 M_\odot$ by setting the axion mass to, $m_B \sim 10^{-22}$eV, and the large dark cores of dwarf galaxies are explained as solitons on the de-Broglie scale. This is persuasive, but detection of the inherent scalar field oscillation at the Compton frequency, $ω_B= (2.5{\rm \, months})^{-1}(m_B/10^{-22}eV)$, would be definitive. By evolving the coupled Schrödinger-Poisson equation for a Bose-Einstein condensate, we predict the dark matter is fully modulated by de-Broglie interference, with a dense soliton core of size $\simeq 150pc$, at the Galactic center. The oscillating field pressure induces General Relativistic time dilation in proportion to the local dark matter density and pulsars within this dense core have detectably large timing residuals, of $\simeq 400nsec/(m_B/10^{-22}eV)$. This is encouraging as many new pulsars should be discovered near the Galactic center with planned radio surveys. More generally, over the whole Galaxy, differences in dark matter density between pairs of pulsars imprints a pairwise Galactocentric signature that can be distinguished from an isotropic gravitational wave background.
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