Abstract We report the detection of an antiglitch with a fractional frequency change of Δ ν / ν = −3.46(6) × 10 −9 in the rotation-powered pulsar PSR J1835−1106 at MJD 55813(9), based on timing observations collected with the Nanshan 26 m and Parkes 64 m radio telescopes from 2000 January to 2022 July. A comparison of the average pulse profiles within ±300 days of the event reveals no significant morphological changes. We also estimate the angular velocity lag between the normal and superfluid components at the time of the glitch, showing that one of the superfluid glitch models is incompatible with PSR J1835−1106 due to its insufficient spin-down rate and angular velocity lag. The wind braking scenario offers a viable alternative, consistent with the observed spin-down behavior, glitch amplitude, and postglitch recovery. High-cadence, high-sensitivity monitoring of similar events is essential to distinguish between internal (superfluid) and external (wind-related) glitch mechanisms.
Wang et al. (Tue,) studied this question.