Location via proxy:   [ UP ]  
[Report a bug]   [Manage cookies]                

Primordial black holes and scalar-induced secondary gravitational waves from inflationary models with a noncanonical kinetic term

Zhu Yi (易竹), Qing Gao (郜青), Yungui Gong (龚云贵), and Zong-hong Zhu (朱宗宏)
Phys. Rev. D 103, 063534 – Published 29 March 2021
PDFHTMLExport Citation
Abstract
Authors
Article Text
  • INTRODUCTION
  • THE ENHANCEMENT MECHANISM
  • HIGGS MODEL
  • T-MODEL
  • CONCLUSION
  • ACKNOWLEDGMENTS
  • APPENDICES
    • References

    Abstract

    With the enhancement mechanism provided by a noncanonical kinetic term with a peak, the amplitude of primordial curvature perturbations can be enhanced by seven orders of magnitude at small scales while keeping to be consistent with observations at large scales. The peak function and inflationary potential are not restricted in this mechanism. We use the Higgs model and T-model as examples to show how abundant primordial black hole dark matter with different mass and scalar induced secondary gravitational waves with different peak frequency are generated. We also show that the enhanced power spectrum for the primordial curvature perturbations and the energy density of the scalar induced secondary gravitational waves can have either a sharp peak or a broad peak. The primordial black holes with the mass around 10−14−10−12  M⊙ produced with the enhancement mechanism can make up almost all dark matter, and the scalar induced secondary gravitational waves accompanied with the production of primordial black holes can be tested by the pulsar timing arrays and spaced based gravitational wave observatory. Therefore, the mechanism can be tested by primordial black hole dark matter and gravitational wave observations.

    • Figure
    • Figure
    • Figure
    • Figure
    • Figure
    • Figure
    • Figure
    • Received 24 November 2020
    • Accepted 8 March 2021

    DOI:https://doi.org/10.1103/PhysRevD.103.063534

    © 2021 American Physical Society

    Physics Subject Headings (PhySH)

    1. Research Areas
    Dark matterGravitational wavesInflation
    Gravitation, Cosmology & Astrophysics

    Authors & Affiliations

    Zhu Yi (易竹)1,‡, Qing Gao (郜青)2,†, Yungui Gong (龚云贵)3,*, and Zong-hong Zhu (朱宗宏)1,§

    • 1Department of Astronomy, Beijing Normal University, Beijing 100875, China
    • 2School of Physical Science and Technology, Southwest University, Chongqing 400715, China
    • 3School of Physics, Huazhong University of Science and Technology, Wuhan, Hubei 430074, China

    • *Corresponding author. yggong@hust.edu.cn
    • †gaoqing1024@swu.edu.cn
    • ‡yz@bnu.edu.cn
    • §zhuzh@bnu.edu.cn

    Article Text (Subscription Required)

    Click to Expand

    References (Subscription Required)

    Click to Expand
    Issue

    Vol. 103, Iss. 6 — 15 March 2021

    Reuse & Permissions
    Access Options
    Author publication services for translation and copyediting assistance advertisement

    Authorization Required

    Log In
    Other Options
    ×

    Images

    • Figure 1
      Figure 1

      The peak function Gp(ϕ) with different q.

      Reuse & Permissions
    • Figure 2
      Figure 2

      The enhanced power spectrum in the Higgs model. The blue and black lines denote the results for the models H11 with sharp peak and H12 with broad peak, respectively. The light green shaded region is excluded by the CMB observations [28]. The yellow, blue, and orange regions show the constraints from the PTA observations [105], the effect on the ratio between neutron and proton during the big bang nucleosynthesis (BBN) [106] and μ-distortion of CMB [107], respectively.

      Reuse & Permissions
    • Figure 3
      Figure 3

      The abundances of PBHs produced in the models H11 and H12. The blue and black lines denote the results for the models H11 and H12, respectively. The shaded regions show the observational constraints on the PBH abundance: the yellow region from accretion constraints by CMB [123, 124], the red region from extragalactic gamma-rays by PBH evaporation (EGγ) [125], the cyan region from galactic center 511 keV gamma-ray line (INTEGRAL) [126, 127, 128], the orange region from white dwarf explosion (WD) [129], the green region from microlensing events with Subaru HSC [130], the blue region from the Kepler satellite [131], the gray region from the EROS/MACHO [132].

      Reuse & Permissions
    • Figure 4
      Figure 4

      The scalar induced secondary GWs for the Higgs model. The blue and black lines denote the models H11 and H12, respectively. The pink dashed curve denotes the EPTA limit [88, 89, 90, 91], the cyan dotted curve denotes the SKA limit [92], the red dot-dashed curve in the middle denotes the TianQin limit [96], the dotted magenta curve shows the Taiji limit [95], the brown dashed curve shows the LISA limit [94], and the gray dot-dashed curve denotes the aLIGO limit [133, 134].

      Reuse & Permissions
    • Figure 5
      Figure 5

      The enhanced power spectrum in the T-model. The blue and black lines denote the results for the models T11 with sharp peak and T12 with broad peak, respectively.

      Reuse & Permissions
    • Figure 6
      Figure 6

      The PBHs abundance for the models display in Fig. 5. The blue and black lines denote the models labeled as T11, T12, respectively.

      Reuse & Permissions
    • Figure 7
      Figure 7

      The SIGWs for the T-model. The blue and black lines denote the models T11 and T12, respectively.

      Reuse & Permissions
    ×

    Sign up to receive regular email alerts from Physical Review D

    Log In

    Cancel
    ×

    Search

    Article Lookup

    Paste a citation or DOI
    Enter a citation
    ×