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We present results of the spectral and timing analysis of the X-ray pulsarLMC X-4 with the NuSTAR observatory in the broad energy range 3-79 keV. Alongwith the detailed analysis of the averaged source spectrum, the high-precisionpulse phased-resolved spectra were obtained for the first time. It has beenshown that the comptonization model gives the best approximation of theobtained spectra. The evolution of its parameters was traced depending on thepulse phase as well. The search for the possible cyclotron absorption line wasperformed for all energy spectra in the 5-55 keV energy range. The obtainedupper limit for the depth of the cyclotron absorption line $\tau\simeq0.15$($3\sigma$) indicates no cyclotron absorption line in this energy range, whichprovides an estimate of the magnitude of the magnetic field on the surface ofthe neutron star: $B < 3 \times 10^{11}$ G or $B > 6.5 \times 10^{12}$ G. Thelatter one is agree with the estimate of the magnetic field obtained from theanalysis of the power spectrum of the pulsar: $B \sim 3 \times 10^{13}$ G.Based on results of the pulse phase-resolved spectroscopy we revealed a delaybetween maxima of the source emission and the equivalent width of thefluorescent iron line. This delay can be apparently associated with the traveltime of photons between the emitting regions in the vicinity of the neutronstar and the relatively cold regions where this emission is reflected(presumably, at the inflowing stream or at the place of an interaction of thestream and the outer edge of the accretion disk).

Observations of the X-ray pulsar LMC X-4 with NuSTAR: limit on the magnetic field and tomography of the system in the fluorescent iron line