Gravitational waves can probe the existence of planetary-mass primordial black holes. Considering a mass range of $[10^{-7}-10^{-2}]M_{\odot }$, inspiraling primordial black holes could emit either continuous gravitational waves, quasi-monochromatic signals that last for many years, or transient continuous waves, signals whose frequency evolution follows a power law and last for $\mathcal{O}$(hours-months). We show that primordial black hole binaries in our galaxy may produce detectable gravitational waves for different mass functions and formation mechanisms. In order to detect these inspirals, we adapt methods originally designed to search for gravitational waves from asymmetrically rotating neutron stars. The first method, the Frequency-Hough, exploits the continuous, quasi-monochromatic nature of inspiraling black holes that are sufficiently light and far apart such that their orbital frequencies can be approximated as linear with a small spin-up. The second method, the Generalized Frequency-Hough, drops the assumption of linearity and allows the signal frequency to follow a power-law evolution. We explore the parameter space to which each method is sensitive, derive a theoretical sensitivity estimate, determine optimal search parameters and calculate the computational cost of all-sky and directed searches. We forecast limits on the abundance of primordial black holes within our galaxy, showing that we can constrain the fraction of dark matter that primordial black holes compose, $f_{\mathrm{PBH}}$, to be $f_{\mathrm{PBH}}\lesssim 1$ for chirp masses between $[4\times 10^{-5}-10^{-3}]M_{\odot }$ for current detectors. For the Einstein Telescope, we expect the constraints to improve to $f_{\mathrm{PBH}}\lesssim 10^{-2}$ for chirp masses between $[10^{-4}-10^{-3}]M_{\odot }$.

引力波可以探测行星质量原始黑洞的存在。考虑到质量范围$[\mathrm{1个}{0}^{-7}-\mathrm{1个}{0}^{-\mathrm{2个}}]{\mathrm{中号}}_{\odot }$，鼓舞人心的原始黑洞可能会发出连续的引力波，持续多年的准单色信号，或者发出瞬态连续波，其频率演化遵循幂律并持续到 $\mathcal{Ø}$（小时-月）。我们表明，我们银河系中的原始黑洞双星可能会为不同的质量函数和形成机制产生可检测到的引力波。为了检测这些吸气，我们采用了最初设计为从不对称旋转的中子星中搜索引力波的方法。第一种方法是“频率霍夫”，它利用了吸气黑洞的连续，准单色性质，这些黑洞足够轻且相距很远，因此它们的轨道频率可以近似地线性化​​，并具有很小的自旋。第二种方法是广义频率霍夫（Generalized Frequency-Hough），它放弃了线性假设，并允许信号频率遵循幂律演变。我们探索每种方法都敏感的参数空间，得出理论上的敏感度估算值，确定最佳搜索参数并计算全天候搜索和定向搜索的计算成本。我们预测了银河系中原始黑洞的丰度极限，这表明我们可以限制原始黑洞组成的暗物质所占的比例，$F_{\mathrm{PBH}}$， 成为 $F_{\mathrm{PBH}}\lesssim \mathrm{1个}$ 对于之间的chi声 $[4\times \mathrm{1个}{0}^{-5}-\mathrm{1个}{0}^{-3}]{\mathrm{中号}}_{\odot }$用于电流检测器。对于爱因斯坦望远镜，我们希望约束条件可以改善为$F_{\mathrm{PBH}}\lesssim \mathrm{1个}{0}^{-\mathrm{2个}}$ 对于之间的chi声 $[\mathrm{1个}{0}^{-4}-\mathrm{1个}{0}^{-3}]{\mathrm{中号}}_{\odot }$。