Baryogenesis and gravitational waves in the ZeeBabu Model
Abstract
The sphaleron process in the baryogensis scenario is calculated, to explain the matterantimatter asymmetry in the ZeeBabu (ZB) model. It always satisfies the decoupling condition and the strength of phase transition ($S$) is always greater than 1 in the presence of triggers other than SM, which are single ($h^{\pm}$) and double ($k^{\pm\pm}$) charged boson. Sphaleron energies are in the range of 510 TeV, when calculated using bubble profiles containing free parameters and assuming nuclear bubbles of $h^{\pm}$ and $k^{\pm\pm}$ are very small. We tested the scaling law of sphaleron again with an average error of $10\%$. When the temperature is close to the critical temperature ($T_C$), the density of nuclear bubble is produced very large and decreases as the temperature decreases. The key parameter is $\alpha$ which results in the gravitational wave density parameter ($\Omega h^2$) in the range of $10^{17}$ to $10^{15}$ when $\beta/H^*=50$, this is not enough to detect gravitational waves from electroweak phase transition (EWPT) according to LISA data. As the larger strength of phase transition is, the more $\alpha$ increases (this increase is almost linear with $S$), the larger the gravitational wave density parameter is. Also in the context of considering the generation of gravitational waves, in the Zee  Babu model we calculated $\alpha \sim \text{a few} \times 10^{2}\ll 1$, so rigorously conclude that the EWPT is not strong even though $S>1$. We also suggest that, for a model with a lot of extra scalar particles and particles which play a role in mass generation, the stronger the EWPT process and the larger $\Omega h^2$ can be.
 Publication:

arXiv eprints
 Pub Date:
 July 2021
 arXiv:
 arXiv:2107.13823
 Bibcode:
 2021arXiv210713823P
 Keywords:

 High Energy Physics  Phenomenology
 EPrint:
 26 Pages, 8 Figures