2025A&A...693A.235S

We report on the discovery and spectroscopic confirmation of TOI-2458 b, a transiting mini-Neptune around an F-type star leaving the main-sequence with a mass of M_★ = 1.05 ± 0.03 M_⊙, a radius of R_★ = 1.31 ± 0.03 R_⊙, an effective temperature of T_eff = 6005 ± 50 K, and a metallicity of -0.10 ± 0.05 dex. By combining TESS photometry with high-resolution spectra acquired with the HARPS spectrograph, we found that the transiting planet has an orbital period of -3.74 days, a mass of M_p = 13.31 ± 0.99 M_⊕ and a radius of R_p = 2.83 ± 0.20 R_⊕. The host star TOI-2458 shows a short activity cycle of ∼54 days revealed in the HARPS S-index and Ha times series. We took the opportunity to investigate other F stars showing activity cycle periods comparable to that of TOI-2458 and found that they have shorter rotation periods than would be expected based on the gyrochronology predictions. In addition, we determined TOI-2458's stellar inclination angle to be ${i_ \star } = 10.6_{ - 10.6}^{ + 13.3}$ degrees. We discuss that both phenomena (fast stellar rotation and planet orbit inclination) could be explained by in situ formation of a hot Jupiter interior to TOI-2458 b. It is plausible that this hot Jupiter was recently engulfed by the star. Analysis of HARPS spectra has identified the presence of another planet with a period of P = 16.55 ± 0.06 days and a minimum mass of M_p sin i = 10.22 ± 1.90 M_⊕. Using dynamical stability analysis, we constrained the mass of this planet to the range M_c ≃ (10, 25) M_⊕.