论文标题
丽莎会从银河宇宙弦环中检测到谐波引力波吗？
Will LISA Detect Harmonic Gravitational Waves from Galactic Cosmic String Loops?
论文作者
论文摘要
近年来，在观察宇宙字符串的观察方面的快速发展对其性质的限制越来越严格，$Gμ\ Lessim 10^{ - 11} $从Pulsar Time Array（PTA）中。由于缓慢的循环衰减和低重力后坐力，宇宙弦线环在银河系中具有低弦张力团块，从而极大地增强了银河系的循环丰度。 With an average separation of down to just a fraction of a kpc, and the total power of gravitational wave (GW) emission dominated by harmonic modes spanning a wide angular scale, resolved loops located in proximity are powerful, persistent, and highly monochromatic sources of GW with a harmonic signature not replicated by any other sources, making them prime targets for direct detection by the upcoming Laser Interferometer Space Antenna （Lisa），其频率范围匹配良好。与检测速率尺度具有循环丰度的检测不同，谐波信号的检测速率是GW发射，循环丰度和其他噪声源之间的复杂相互作用的结果，并且通过数值模拟来最适当地研究。我们开发了一个可靠，灵活的框架，用于模拟星系中的环路，以预测LISA从解析环中直接检测谐波信号。我们的模拟表明，参数空间中最容易访问的区域由大环组成$α= 0.1 $，低张力$ 10^{ - 21} \ LessimgμGμ\ Lessim 10^{ - 19} $。直接检测场理论宇宙字符串不太可能，而检测概率$ p _ {\ mathrm {det}}} \ Lessim 2 \％$用于一年的任务。扩展表明，直接检测具有低信誉概率的宇宙超链是非常有希望的。通过LISA观察搜索从解决循环中搜索谐波GW信号，可能会在字符串理论上施加物理限制。
Rapid advancement in the observation of cosmic strings has been made in recent years placing increasingly stringent constraints on their properties, with $Gμ\lesssim 10^{-11}$ from Pulsar Timing Array (PTA). Cosmic string loops with low string tension clump in the Galaxy due to slow loop decay and low gravitational recoil, resulting in great enhancement to loop abundance in the Galaxy. With an average separation of down to just a fraction of a kpc, and the total power of gravitational wave (GW) emission dominated by harmonic modes spanning a wide angular scale, resolved loops located in proximity are powerful, persistent, and highly monochromatic sources of GW with a harmonic signature not replicated by any other sources, making them prime targets for direct detection by the upcoming Laser Interferometer Space Antenna (LISA), whose frequency range is well-matched. Unlike detection of bursts where the detection rate scales with loop abundance, the detection rate for harmonic signal is the result of a complex interplay between the strength of GW emission, loop abundance, and other sources of noise, and is most suitably studied through numerical simulations. We develop a robust and flexible framework for simulating loops in the Galaxy for predicting direct detection of harmonic signal from resolved loops by LISA. Our simulation reveals that the most accessible region in the parameter space consists of large loops $α=0.1$ with low tension $10^{-21}\lesssim Gμ\lesssim 10^{-19}$. Direct detection of field theory cosmic strings is unlikely, with the detection probability $p_{\mathrm{det}}\lesssim 2\%$ for a 1-year mission. An extension suggests that direct detection of cosmic superstrings with a low intercommutation probability is very promising. Searching for harmonic GW signal from resolved loops through LISA observations will potentially place physical constraints on string theory.
