The interpretation of pulsar rotational glitches, the sudden increase in spin frequency of
neutron stars, is a half-century-old challenge. The common view is that glitches are driven by …

Young and rotation-powered neutron stars (NSs) are commonly observed as rapidly-
spinning pulsars. They dissipate their rotational energy by emitting pulsar wind with …

We present a phase-coherent timing solution for PSR J1640–4631, a young 206 ms pulsar
using X-ray timing observations taken with NuSTAR. Over this timing campaign, we have …

The location of radio pulsars in the period–period derivative (P–) plane has been a key
diagnostic tool since the early days of pulsar astronomy. Of particular importance is how …

Radio pulsars are believed to have their emission powered by the loss of rotational kinetic
energy. By contrast, magnetars show intense X-ray and γ-ray radiation whose luminosity …

The young, fast-spinning X-ray pulsar J0537− 6910 displays an extreme glitch activity, with
large spin-ups interrupting its decelerating rotation every∼ 100 d. We present nearly 13 yr of …

We have observed a large glitch in the Crab pulsar (PSR B0531+ 21). The glitch occurred
around MJD 58064 (2017 November 8) when the pulsar underwent an increase in the …

Magnetic field evolution in neutron-star crusts is driven by the Hall effect and Ohmic
dissipation, for as long as the crust is sufficiently strong to absorb Maxwell stresses exerted …

We analyzed broadband X-ray and radio data of the magnetar SGR J1935+ 2154 taken in
the aftermath of its 2014, 2015, and 2016 outbursts. The source soft X-ray spectrum< 10 keV …

Because of the lack of long-term pulsed emission in quiescence and the strong timing noise,
it is impossible to directly measure the braking index n of a magnetar. Based on the …