Nustar observation of the binary system 4U 0114+65

Abstract

The high mass X-ray binary system 4U 0114+65 was observed by Nustar in October 2019, and by XMM-Newton in August 2015. Here we performed spectral and timing analysis of the Nustar observation, and carry out timing analysis on the XMM-Newton data. We measured the spin period of the neutron star from both observations and found a spin-up rate $\dot{p}=1.54\pm 0.38\times 10^{-6}s{s}^{-1}$. During the Nustar observation two flares occured, one occured shortly after the start of the observation and the other near the end separated by a long period of low/quiescent- state. The large and sudden flares mostly resulted from accretion of Corotating Interaction Region (CIR) material. A common spectral model to HMXBs, powerlaw with high energy cutoff and absorption at low energy, gave a good fit to both flaring and quiescent states. A flourescent iron line was not required in fitting any of the states. On the other hand, very tentative evidence of Cyclotron Resonant Scattering Feature (CRSF) at $\sim$ 17 keV was found during fitting using cyclabs model, however fitting improvement was not significant enough to confirm its detection, plus a very narrow width (< 1 keV) was obtained for the line and its first harmonic. Visual inspection of the spectra showed a deficiency of emission near the expected first and second harmonic. Another important feature visually noticed in the spectra is the presence of hard tail above 50 keV. This could be explained by the shocked material bounding the CIR.

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Cited by in corpus (1)

• Cyclical accretion regime change in the slow X-ray pulsar 4U 0114+65 observed with Chandra