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  • Letter
  • Open Access

Gravitational wave production from axion rotations right after a transition to kination

Keisuke Harigaya1,2,3, Keisuke Inomata2, and Takahiro Terada4

  • 1Department of Physics, University of Chicago, Chicago, Illinois 60637, USA
  • 2Kavli Institute for Cosmological Physics and Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA
  • 3Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
  • 4Particle Theory and Cosmology Group, Center for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon 34126, Korea

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Phys. Rev. D 108, L081303 – Published 23 October, 2023

DOI: https://doi.org/10.1103/PhysRevD.108.L081303

Abstract

Rotations of axion fields in the early Universe can produce dark matter and the matter-antimatter asymmetry of the Universe. We point out that the rotation can generate an observable amount of a stochastic gravitational wave (GW) background. It can be doubly enhanced in a class of models in which the equation of state of the rotations rapidly changes from a nonrelativistic matterlike one to a kinationlike one by (1) the so-called poltergeist mechanism and (2) slower redshift of GWs compared to the axion-kination fluid. In supersymmetric UV completion, future GW observations can probe the supersymmetry-breaking scale up to 107  GeV even if the axion does not directly couple to the Standard Model fields.

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References (78)

  1. C. Caprini et al., J. Cosmol. Astropart. Phys. 04 (2016) 001.
  2. C. Caprini and D. G. Figueroa, Classical Quantum Gravity 35, 163001 (2018).
  3. C. Caprini et al., J. Cosmol. Astropart. Phys. 03 (2020) 024.
  4. P. Auclair et al. (LISA Cosmology Working Group), Living Rev. Relativity 26, 5 (2023).
  5. R. D. Peccei and H. R. Quinn, Phys. Rev. Lett. 38, 1440 (1977).
  6. R. D. Peccei and H. R. Quinn, Phys. Rev. D 16, 1791 (1977).
  7. Y. Chikashige, R. N. Mohapatra, and R. D. Peccei, Phys. Lett. 98B, 265 (1981).
  8. C. D. Froggatt and H. B. Nielsen, Nucl. Phys. B147, 277 (1979).
  9. Y. Nambu and G. Jona-Lasinio, Phys. Rev. 122, 345 (1961).
  10. J. Goldstone, Nuovo Cimento 19, 154 (1961).
  11. J. Goldstone, A. Salam, and S. Weinberg, Phys. Rev. 127, 965 (1962).
  12. S. Weinberg, Phys. Rev. Lett. 40, 223 (1978).
  13. F. Wilczek, Phys. Rev. Lett. 40, 279 (1978).
  14. J. Preskill, M. B. Wise, and F. Wilczek, Phys. Lett. 120B, 127 (1983).
  15. L. F. Abbott and P. Sikivie, Phys. Lett. 120B, 133 (1983).
  16. M. Dine and W. Fischler, Phys. Lett. 120B, 137 (1983).
  17. C. B. Adams et al., arXiv:2203.14923.
  18. I. Affleck and M. Dine, Nucl. Phys. B249, 361 (1985).
  19. K. Kamada and C. S. Shin, J. High Energy Phys. 04 (2020) 185.
  20. R. T. Co, L. J. Hall, and K. Harigaya, Phys. Rev. Lett. 124, 251802 (2020).
  21. R. T. Co, L. J. Hall, and K. Harigaya, J. High Energy Phys. 01 (2021) 172.
  22. R. T. Co, K. Harigaya, and A. Pierce, J. Cosmol. Astropart. Phys. 10 (2022) 037.
  23. C. Eröncel and G. Servant, J. Cosmol. Astropart. Phys. 01 (2023) 009.
  24. R. T. Co, L. J. Hall, K. Harigaya, K. A. Olive, and S. Verner, J. Cosmol. Astropart. Phys. 08 (2020) 036.
  25. R. T. Co, K. Harigaya, and A. Pierce, J. High Energy Phys. 12 (2021) 099.
  26. C. Eröncel, R. Sato, G. Servant, and P. Sørensen, J. Cosmol. Astropart. Phys. 10 (2022) 053.
  27. A. Arvanitaki, S. Dimopoulos, M. Galanis, L. Lehner, J. O. Thompson, and K. Van Tilburg, Phys. Rev. D 101, 083014 (2020).
  28. R. T. Co and K. Harigaya, Phys. Rev. Lett. 124, 111602 (2020).
  29. R. T. Co, N. Fernandez, A. Ghalsasi, L. J. Hall, and K. Harigaya, J. High Energy Phys. 03 (2021) 017.
  30. K. Harigaya and I. R. Wang, J. High Energy Phys. 10 (2021) 022; 12 (2021) 193(E).
  31. S. Chakraborty, T. H. Jung, and T. Okui, Phys. Rev. D 105, 015024 (2022).
  32. J. Kawamura and S. Raby, J. High Energy Phys. 04 (2022) 116.
  33. R. T. Co, K. Harigaya, Z. Johnson, and A. Pierce, J. High Energy Phys. 11 (2021) 210.
  34. P. Barnes, R. T. Co, K. Harigaya, and A. Pierce, J. High Energy Phys. 05 (2023) 114.
  35. R. T. Co, V. Domcke, and K. Harigaya, J. High Energy Phys. 07 (2023) 179.
  36. M. Badziak and K. Harigaya, J. High Energy Phys. 06 (2023) 014.
  37. R. T. Co, D. Dunsky, N. Fernandez, A. Ghalsasi, L. J. Hall, K. Harigaya, and J. Shelton, J. High Energy Phys. 09 (2022) 116.
  38. Y. Gouttenoire, G. Servant, and P. Simakachorn, arXiv:2108.10328.
  39. Y. Gouttenoire, G. Servant, and P. Simakachorn, arXiv:2111.01150.
  40. E. Madge, W. Ratzinger, D. Schmitt, and P. Schwaller, SciPost Phys. 12, 171 (2022).
  41. B. Spokoiny, Phys. Lett. B 315, 40 (1993).
  42. M. Joyce, Phys. Rev. D 55, 1875 (1997).
  43. P. G. Ferreira and M. Joyce, Phys. Rev. D 58, 023503 (1998).
  44. K. Inomata, K. Kohri, T. Nakama, and T. Terada, Phys. Rev. D 100, 043532 (2019).
  45. K. Inomata, M. Kawasaki, K. Mukaida, T. Terada, and T. T. Yanagida, Phys. Rev. D 101, 123533 (2020).
  46. G. White, L. Pearce, D. Vagie, and A. Kusenko, Phys. Rev. Lett. 127, 181601 (2021).
  47. G. Domènech, C. Lin, and M. Sasaki, J. Cosmol. Astropart. Phys. 04 (2021) 062; 11 (2021) E01.
  48. G. Domènech, V. Takhistov, and M. Sasaki, Phys. Lett. B 823, 136722 (2021).
  49. K. D. Lozanov and V. Takhistov, Phys. Rev. Lett. 130, 181002 (2023).
  50. N. Bhaumik, A. Ghoshal, and M. Lewicki, J. High Energy Phys. 07 (2022) 130.
  51. N. Bhaumik, A. Ghoshal, R. K. Jain, and M. Lewicki, J. High Energy Phys. 05 (2023) 169.
  52. S. Kasuya, M. Kawasaki, and K. Murai, J. Cosmol. Astropart. Phys. 05 (2023) 053.
  53. G. Domènech and M. Sasaki, Classical Quantum Gravity 40, 177001 (2023).
  54. G. Domènech, Int. J. Mod. Phys. D 29, 2050028 (2020).
  55. G. Domènech, S. Pi, and M. Sasaki, J. Cosmol. Astropart. Phys. 08 (2020) 017.
  56. S. Weinberg, Cosmology (Oxford University Press, New York, 2008).
  57. K. N. Ananda, C. Clarkson, and D. Wands, Phys. Rev. D 75, 123518 (2007).
  58. D. Baumann, P. J. Steinhardt, K. Takahashi, and K. Ichiki, Phys. Rev. D 76, 084019 (2007).
  59. See Supplemental Material at http://link.aps.org/supplemental/10.1103/PhysRevD.108.L081303 not only for the definition of the Fourier mode of the tensor perturbations, but also for a review of equations of motion for a rotating field and two-field model, the detailed calculation of the evolution of the background and perturbation quantities, and induced GWs, and the discussion on the limitation of the linear analysis.
  60. V. Mukhanov, Physical Foundations of Cosmology (Cambridge University Press, Cambridge, England, 2005).
  61. H. Assadullahi and D. Wands, Phys. Rev. D 79, 083511 (2009).
  62. K. Kohri and T. Terada, Phys. Rev. D 97, 123532 (2018).
  63. K. Inomata, K. Kohri, T. Nakama, and T. Terada, J. Cosmol. Astropart. Phys. 10 (2019) 071.
  64. M. Laine and M. E. Shaposhnikov, Nucl. Phys. B532, 376 (1998).
  65. V. Domcke, K. Harigaya, and K. Mukaida, J. High Energy Phys. 08 (2022) 234.
  66. P. Adshead and W. Hu, Phys. Rev. D 89, 083531 (2014).
  67. K. Inomata, E. McDonough, and W. Hu, Phys. Rev. D 104, 123553 (2021).
  68. K. Inomata, E. McDonough, and W. Hu, J. Cosmol. Astropart. Phys. 02 (2022) 031.
  69. K. Schmitz, J. High Energy Phys. 01 (2021) 097.
  70. S. Kawamura et al., Prog. Theor. Exp. Phys. 2021, 05A105 (2021).
  71. M. J. Dolan, F. J. Hiskens, and R. R. Volkas, J. Cosmol. Astropart. Phys. 10 (2022) 096.
  72. M. Kawasaki and K. Murai, arXiv:2308.13134.
  73. K. Jedamzik, M. Lemoine, and J. Martin, J. Cosmol. Astropart. Phys. 09 (2010) 034.
  74. K. Jedamzik, M. Lemoine, and J. Martin, J. Cosmol. Astropart. Phys. 04 (2010) 021.
  75. M. Yu. Khlopov and A. G. Polnarev, Phys. Lett. 97B, 383 (1980).
  76. A. G. Polnarev and M. Yu. Khlopov, Sov. Astron. 26, 9 (1982).
  77. T. Harada, C.-M. Yoo, K. Kohri, K.-i. Nakao, and S. Jhingan, Astrophys. J. 833, 61 (2016).
  78. T. Harada, C.-M. Yoo, K. Kohri, and K.-I. Nakao, Phys. Rev. D 96, 083517 (2017).

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Phys. Rev. D 108, L081303– Published 23 October, 2023
  • Received 6 June 2023
  • Accepted 29 September 2023
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