Abstract
We report on the XMM-Newton observations of the redback pulsar PSR J2339−0533. For the X-ray emission we found confirmation for a binary-phase dependence. The emission appears to be orbitally modulated at the 4.6-hour orbital period, with two peaks and two dips, where the dips concurred by a softening in the spectrum. We suggest that the X-rays could be decomposed into a hard variable component plus a soft-steady component. The broad band (0.5 − 8.0 keV) binary-phase resolved spectral analysis discloses a thermal X-ray component (< 30%) of the emission from PSR J2339−0533 at various orbital phases, confirming the results from previous studies. We conclude that the majority of X-ray emissions are from a power-law component and can be attributed to intra-binary shock emission from the interface between pulsar wind and the ablated material from the secondary star. We also report non-detection of pulsation on various X-ray energy bands; we did not find any pulsation at the gamma-ray/radio timing solution. The geometry of the binary configuration is explored in our study. We explain the shape of the orbitally phase-folded lightcurve with the Doppler boosting model, concluding that the shock is possibly located near the inner Lagrangian point (L1). By exploring the energetics of the system, we infer that the shock emission at the shock front favors a magnetically-dominated (σ ≫ 1) pulsar wind. Lastly we discuss the possibility of the presence of an accretion disk on the time of observation.