We presented a comprehensive multi-epoch timing and multiwavelength analysis of the accreting millisecond X-ray pulsar (∋cer), we found the spin frequency and orbital parameters from the observations in 0. 3--5 keV. For the 2025 outburst, we reported the detection of pulsations with the (EP). Based on the ∼3-year baseline between these two outbursts, we measured a significant long-term spin-down rate of dotν = (-5. 73 ± 0. 28) covering two major outbursts in 2022 and 2025. By reanalyzing the 2022 outburst data from the Neutron Star Interior Composition Explorer Einstein Probe 10^ -14 ̊m Hz s^ -1. Assuming that the quiescent spin-down is driven by magnetic dipole radiation, we inferred a spin-down luminosity of L ≈ 1. 1 10^ 36 ̊m erg s^ -1 and a surface dipolar magnetic field of B ≈ (7. 3 - 10. 4) (FAST) during the X-ray quiescent state in 2024, resulting in a non-detection with a 7σ flux density upper limit of 12. 3 μJy. This corresponds to a radio efficiency upper limit of ξ < 2. 8, which is significantly lower than that of typical millisecond pulsars with a similar spin-down power. This profound radio pulsation faintness can be explained by two primary scenarios: either a geometric effect, wherein the pulsar's radio beam is directed away from our line of sight, or a physical suppression of the emission mechanism, potentially caused by a persistent low-level accretion flow during the X-ray quiescent state. 10⁸ G. Furthermore, we conducted a deep radio pulsation search with the Five-hundred-meter Aperture Spherical radio Telescope 10^ -10
Li et al. (Wed,) studied this question.