- Letter
- Open Access
Standard model violation is enough
Phys. Rev. D 112, L011701 – Published 2 July, 2025
DOI: https://doi.org/10.1103/glgl-v4v6
Abstract
Is the standard model charge-parity () violation ever enough to generate the observed baryon asymmetry? Yes! We introduce a mechanism of baryogenesis (and dark matter production) that can generate the entire observed baryon asymmetry of the Universe using only the violation within standard model systems—a feat which no other mechanism currently proposed can achieve. Baryogenesis proceeds through a mesogenesis scenario but with well motivated additional dark sector dynamics: a morphon field generates present day mass contributions for the particle mediating the decay responsible for baryogenesis. The effect is an enhancement of baryon production while evading present day collider constraints. The violation comes entirely from standard model contributions to neutral meson systems. Meanwhile, the dark dynamics generate gravitational waves that may be searched for with current and upcoming pulsar timing arrays, as we demonstrate with an example potential that is tuned to generate domain walls that annihilate later. This mechanism, mesogenesis with a morphing mediator, motivates probing a new parameter space as well as improving the sensitivity of existing mesogenesis searches at hadron and electron colliders.
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References (52)
- A. D. Sakharov, Pis’ma Zh. Eksp. Teor. Fiz. 5, 32 (1967).
- C. Jarlskog, Phys. Rev. Lett. 55, 1039 (1985).
- M. B. Gavela, P. Hernandez, J. Orloff, and O. Pene, Mod. Phys. Lett. A 9, 795 (1994).
- M. B. Gavela, M. Lozano, J. Orloff, and O. Pene, Nucl. Phys. B430, 345 (1994).
- M. B. Gavela, P. Hernandez, J. Orloff, O. Pene, and C. Quimbay, Nucl. Phys. B430, 382 (1994).
- P. Huet, in 1994 Meeting of the American Physical Society, Division of Particles and Fields (DPF 94) (World Scientific Pub Co Inc., Singapore, 1994), pp. 1377–1380, https://inspirehep.net/conferences/968643?ui-citation-summary=true.
- P. Huet and E. Sather, Phys. Rev. D 51, 379 (1995).
- M. Berkooz, Y. Nir, and T. Volansky, Phys. Rev. Lett. 93, 051301 (2004).
- G. Perez and T. Volansky, Phys. Rev. D 72, 103522 (2005).
- S. Bruggisser, T. Konstandin, and G. Servant, J. Cosmol. Astropart. Phys. 11 (2017) 034.
- I. Baldes, T. Konstandin, and G. Servant, J. High Energy Phys. 12 (2016) 073.
- B. von Harling and G. Servant, J. High Energy Phys. 05 (2017) 077.
- S. Bruggisser, B. von Harling, O. Matsedonskyi, and G. Servant, Phys. Rev. Lett. 121, 131801 (2018).
- I. Baldes, T. Konstandin, and G. Servant, Phys. Lett. B 786, 373 (2018).
- S. Bruggisser, B. von Harling, O. Matsedonskyi, and G. Servant, J. High Energy Phys. 12 (2018) 099.
- K. Fuyuto, W.-S. Hou, and E. Senaha, Phys. Lett. B 776, 402 (2018).
- F. Elahi, G. Elor, and R. McGehee, Phys. Rev. D 105, 055024 (2022).
- G. Elor and R. McGehee, Phys. Rev. D 103, 035005 (2021).
- G. Elor, M. Escudero, and A. Nelson, Phys. Rev. D 99, 035031 (2019).
- J. Berger and G. Elor, Phys. Rev. Lett. 132, 081002 (2024).
- G. Elor and A. W. M. Guerrera, J. High Energy Phys. 02 (2023) 100.
- G. Alonso-Álvarez, G. Elor, and M. Escudero, Phys. Rev. D 104, 035028 (2021).
- M. Borsato et al., Rep. Prog. Phys. 85, 024201 (2022).
- G. Alonso-Álvarez, G. Elor, M. Escudero, B. Fornal, B. Grinstein, and J. Martin Camalich, Phys. Rev. D 105, 115005 (2022).
- A. Lenz and G. Tetlalmatzi-Xolocotzi, J. High Energy Phys. 07 (2020) 177.
- G. Alonso-Álvarez, G. Elor, A. E. Nelson, and H. Xiao, J. High Energy Phys. 03 (2020) 046.
- P. A. R. Ade et al. (Planck Collaboration), Astron. Astrophys. 594, A13 (2016).
- N. Aghanim et al. (Planck Collaboration), Astron. Astrophys. 641, A6 (2020).
- R. H. Cyburt, B. D. Fields, K. A. Olive, and T.-H. Yeh, Rev. Mod. Phys. 88, 015004 (2016).
- M. Tanabashi et al. (Particle Data Group), Phys. Rev. D 98, 030001 (2018).
- C. Hadjivasiliou et al. (Belle Collaboration), Phys. Rev. D 105, L051101 (2022).
- J. P. Lees et al. (BABAR Collaboration, Phys. Rev. D 107, 092001 (2023).
- G. Elor, R. Houtz, S. Ipek, and M. Ulloa (to be published).
- G. B. Gelmini, M. Gleiser, and E. W. Kolb, Phys. Rev. D 39, 1558 (1989).
- G. B. Gelmini, S. Pascoli, E. Vitagliano, and Y.-L. Zhou, J. Cosmol. Astropart. Phys. 02 (2021) 032.
- J. Preskill, S. P. Trivedi, F. Wilczek, and M. B. Wise, Nucl. Phys. B363, 207 (1991).
- A. Vilenkin, Phys. Rev. D 23, 852 (1981).
- M. Gleiser and R. Roberts, Phys. Rev. Lett. 81, 5497 (1998).
- T. Hiramatsu, M. Kawasaki, and K. Saikawa, J. Cosmol. Astropart. Phys. 05 (2010) 032.
- M. Kawasaki and K. Saikawa, J. Cosmol. Astropart. Phys. 09 (2011) 008.
- D. Stauffer, Phys. Rep. 54, 1 (1979).
- T. Hiramatsu, M. Kawasaki, and K. Saikawa, J. Cosmol. Astropart. Phys. 02 (2014) 031.
- L. Lentati et al. (EPTA Collaboration), Mon. Not. R. Astron. Soc. 453, 2576 (2015).
- G. Janssen et al., Proc. Sci. AASKA14 (2015) 037 [arXiv:1501.00127].
- J. Garcia-Bellido, H. Murayama, and G. White, J. Cosmol. Astropart. Phys. 12 (2021) 023.
- G. Agazie et al. (NANOGrav Collaboration), Astrophys. J. Lett. 951, L8 (2023).
- A. Afzal et al. (NANOGrav Collaboration), Astrophys. J. Lett. 951, L11 (2023); 971, L27(E) (2024).
- F. Riva, Phys. Lett. B 690, 443 (2010).
- S. Antusch and D. Nolde, J. Cosmol. Astropart. Phys. 10 (2013) 028.
- P. Schwaller, Phys. Rev. Lett. 115, 181101 (2015).
- F. Niedermann and M. S. Sloth, The Hubble Constant Tension (Springer, Singapore, 2024).
- R. Fardon, A. E. Nelson, and N. Weiner, J. Cosmol. Astropart. Phys. 10 (2004) 005.