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Detectable Gravitational Wave Signals from Affleck-Dine Baryogenesis

Graham White1,*, Lauren Pearce2,†, Daniel Vagie3,‡, and Alexander Kusenko4,1,§

  • 1Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
  • 2Pennsylvania State University-New Kensington, New Kensington, Pennsylvania 15068, USA
  • 3Department of Physics and Astronomy, University of Oklahoma, Norman, Oklahoma 73019, USA
  • 4Department of Physics and Astronomy, University of California, Los Angeles, Los Angeles, California 90095, USA

  • *graham.white@ipmu.jp
  • †lpearce@psu.edu
  • ‡daniel.d.vagie-1@ou.edu
  • §kusenko@g.ucla.edu
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Phys. Rev. Lett. 127, 181601 – Published 27 October, 2021

DOI: https://doi.org/10.1103/PhysRevLett.127.181601

Abstract

In Affleck-Dine baryogenesis, the observed baryon asymmetry of the Universe is generated through the evolution of the vacuum expectation value of a scalar condensate. This scalar condensate generically fragments into nontopological solitons (Q balls). If they are sufficiently long-lived, they lead to an early matter domination epoch, which enhances the primordial gravitational wave signal for modes that enter the horizon during this epoch. The sudden decay of the Q balls results in a rapid transition from matter to radiation domination, producing a sharp peak in the gravitational wave power spectrum. Avoiding the gravitino over-abundance problem favors scenarios where the peak frequency of the resonance is within the range of the Einstein telescope and/or DECIGO. This observable signal provides a mechanism to test Affleck-Dine baryogenesis.

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Phys. Rev. Lett. 127, 181601– Published 27 October, 2021
  • Received 9 June 2021
  • Accepted 1 October 2021
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