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Rapid advancement in the observation of cosmic strings has been made inrecent years placing increasingly stringent constraints on their properties,with $G\mu\lesssim 10^{-11}$ from Pulsar Timing Array (PTA). Cosmic stringloops with low string tension clump in the Galaxy due to slow loop decay andlow gravitational recoil, resulting in great enhancement to loop abundance inthe Galaxy. With an average separation of down to just a fraction of a kpc, andthe total power of gravitational wave (GW) emission dominated by harmonic modesspanning a wide angular scale, resolved loops located in proximity arepowerful, persistent, and highly monochromatic sources of GW with a harmonicsignature not replicated by any other sources, making them prime targets fordirect detection by the upcoming Laser Interferometer Space Antenna (LISA),whose frequency range is well-matched. Unlike detection of bursts where thedetection rate scales with loop abundance, the detection rate for harmonicsignal is the result of a complex interplay between the strength of GWemission, loop abundance, and other sources of noise, and is most suitablystudied through numerical simulations. We develop a robust and flexibleframework for simulating loops in the Galaxy for predicting direct detection ofharmonic signal from resolved loops by LISA. Our simulation reveals that themost accessible region in the parameter space consists of large loops$\alpha=0.1$ with low tension $10^{-21}\lesssim G\mu\lesssim 10^{-19}$. Directdetection of field theory cosmic strings is unlikely, with the detectionprobability $p_{\mathrm{det}}\lesssim 2\%$ for a 1-year mission. An extensionsuggests that direct detection of cosmic superstrings with a lowintercommutation probability is very promising. Searching for harmonic GWsignal from resolved loops through LISA observations will potentially placephysical constraints on string theory.

Will LISA Detect Harmonic Gravitational Waves from Galactic Cosmic String Loops?