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首页> 外文期刊>Physical review letters >Primordial Black Hole Dark Matter: LISA Serendipity
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Primordial Black Hole Dark Matter: LISA Serendipity

机译：原始的黑洞暗物质：LISA偶然

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摘要

There has recently been renewed interest in the possibility that the dark matter in the Universe consists of primordial black holes (PBHs). Current observational constraints leave only a few PBH mass ranges for this possibility. One of them is around 10(-12) M-circle dot. if PBHs with this mass are formed due to an enhanced scalar-perturbation amplitude, their formation is inevitably accompanied by the generation of gravitational waves (GWs) with frequency peaked in the mHz range, precisely around the maximum sensitivity of the LISA mission. We show that, if these primordial black holes are the dark matter, LISA will be able to detect the associated GW power spectrum. Although the GW source signal is intrinsically non-Gaussian, the signal measured by LISA is a sum of the signal from a large number of independent sources suppressing the non-Gaussianity at detection to an unobservable level. We also discuss the effect of the GW propagation in the perturbed Universe. PBH dark matter generically leads to a detectable, purely isotropic, Gaussian and unpolarized GW signal, a prediction that is testable with LISA.
机译：最近，人们对宇宙中的暗物质由原始黑洞（PBH）组成的可能性重新引起了兴趣。当前的观测限制只为这种可能性留下了几个PBH质量范围。其中之一是大约10（-12）个M圆点。如果具有这种质量的PBH是由于标量摄动幅度的增加而形成的，则它们的形成不可避免地会伴随着频率在mHz范围内峰值的重力波（GWs）的产生，正好在LISA任务的最大灵敏度附近。我们证明，如果这些原始黑洞是暗物质，则LISA将能够检测到相关的GW功率谱。尽管GW源信号本质上是非高斯信号，但LISA测量的信号是来自大量独立源的信号之和，这些信号将检测时的非高斯信号抑制到无法观察的水平。我们还将讨论GW在受干扰的宇宙中传播的影响。 PBH暗物质通常会导致可检测到的，各向同性的，高斯和非极化的GW信号，这一预测可以通过LISA进行测试。

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  • 来源
    《Physical review letters》 |2019年第21期|211301.1-211301.6|共6页
  • 作者

    Bartolo N.; De Luca V.; Franciolini G.; Lewis A.; Peloso M.; Riotto A.;

  • 作者单位

    Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy|Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy|INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy;

    Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland|Univ Geneva, CAP, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland;

    Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland|Univ Geneva, CAP, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland;

    Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England;

    Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy|Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy;

    Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland|Univ Geneva, CAP, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland;

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