Study on high-frequency quasi-periodic oscillations in rotating black bounce spacetime

Abstract This study investigates the dynamical effects of particles orbiting a celestial body in rotating Simpson-Visser (RSV) spacetime. The results show that, compared to Kerr and rotating regular black holes, the innermost stable circular orbit (ISCO) of an RSV wormhole is closer to the central object. Using high-frequency quasi-periodic oscillation (HFQPO) data from microquasars and $\chi^2$ analysis, we constrain the spin of microquasars and the regularization parameter $l$ in RSV spacetime based on four HFQPO models and their variants, and evaluate the models using the Akaike Information Criterion and Bayes factor.
 Calculations indicate that $\mathrm{ER}_0$, $\mathrm{ER}_1$, $\mathrm{ER}_2$, $\mathrm{RP}_0$, $\mathrm{RP}_2$, and $\mathrm{WD}$ models have the same support by observational data as the best model $\mathrm{TD}$. Other models considered in this paper have less or no support from observational data. Concretely, for cases of $\mathrm{ER}_0$ and $\mathrm{RP}_0$ models, the observational constraints on RSV regularization parameter are respectively: $l^* = 0.908_{-0.073}^{+0.086}$ and $l^* <0.314$ at $68 \%$ confidence level, which correspond to the regular or the Kerr ($l^*=0$) BH. For $\mathrm{ER}_1$, $\mathrm{ER}_2$, $\mathrm{RP}_2$, $\mathrm{TD}$, and $\mathrm{WD}$ models, the observational data suggest that RSV objects should be the traversable wormhole, e.g. we have the limits: $l^* =1.850 \pm 0.036$, $l^* =4.964 \pm 0.046$, etc.