M. Y. Ge

X-Ray Phase-resolved Spectroscopy of PSRs B0531+21, B1509–58, and B0540–69 with RXTE

The Rossi X-Ray Timing Explorer (RXTE) has made hundreds of observations on three famous young pulsars (PSRs) B0531+21 (Crab), B1509-58, and B0540-69. Using the archive RXTE data, we have studied the phase-resolved spectral properties of these pulsars in details. The variation of the X-ray spectrum with phase of PSR B0531+21 is confirmed here much more precisely and more details are revealed than in the previous studies: The spectrum softens from the beginning of the first pulse, turns to harden right at the pulse peak and becomes the hardest at the bottom of the bridge, softens gradually until the second peak, and then softens rapidly. Different from the previous studies, we found that the spectrum of PSR B1509-58 is significantly harder in the center of the pulse, which is also in contrast to that of PSR B0531+21. The variation of the X-ray spectrum of PSR B0540-69 seems similar to that of PSR B1509-58, but with a lower significance. Using about 10 years of data span, we also studied the real time evolution of the spectra of these pulsars, and no significant evolution has been detected. We discuss the constraints of these results on theoretical models of pulsar X-ray emission.

Swift Observations of SMC X-3 during Its 2016–2017 Super-Eddington Outburst

The Be X-ray pulsar, SMC X-3 underwent a giant outburst from 2016 August to 2017 March, which was monitored with the Swift satellite. During the outburst, its broadband flux increased dramatically, and the unabsorbed X-ray luminosity reached an extreme value of

The Optical/UV Excess of X-Ray-dim Isolated Neutron Stars. I. Bremsstrahlung Emission from a Strangeon Star Atmosphere

\sim 10^{39}

EVOLUTION OF THE X-RAY PROFILE OF THE CRAB PULSAR

erg/s around August 24. Using the Swift/XRT data, we measure the observed pulse frequency of the neutron star to compute the orbital parameters of the binary system. After applying the orbital corrections to Swift observations, we find that the spin frequency increases steadily from 128.02 mHz on August 10 and approach to spin equilibrium

Cross-correlations between soft and hard light curves depending on luminosity in the transient neutron star XTE J1701-462

\sim 128.74

A timing view of the heartbeat state of GRS 1915+105

mHz in 2017 January with an unabsorbed luminosity of

The variability classes in IGR J17091–3624 during the 2011 outburst

L_{\rm X} \sim 2\times10^{37}

REVERSE-SHOCK IN TYCHO’S SUPERNOVA REMNANT

erg/s, indicating a strong dipolar magnetic field

Time Evolution of the X-Ray and γ-Ray Fluxes of the Crab Pulsar

B \sim 6.8\times10^{12}

Calvera: A Low-mass Strangeon Star Torqued by Debris Disk?

G at the neutron star surface. The spin-up rate is tightly correlated with its X-ray luminosity during the super-Eddington outburst. The pulse profile in the Swift/XRT data is variable, showing double peaks at the early stage of outburst and then merging into a single peak at low luminosity. Additionally, we report that a low temperature (