Phase-Resolved Spectroscopy of the Magnetar SGR J1745-2900 Based on Data from the NuSTAR Observatory

TL;DR

This study uses NuSTAR data to analyze the phase-resolved X-ray spectra of magnetar SGR J1745-2900, revealing stable emission temperatures but varying apparent sizes of emitting regions during its pulse cycle.

Contribution

It provides detailed phase-resolved spectroscopy of SGR J1745-2900 in the 3-40 keV range, highlighting the stability of temperature and the variation in size of emission regions.

Findings

Pulsed fraction increases slightly as flux decreases.

Temperature of emitting regions remains stable during pulse.

Apparent size of emission regions varies significantly with phase.

Abstract

The magnetar SGR J1745-2900 located in the vicinity of the supermassive black hole Sgr A$^{\star}$ was detected during its X-ray outburst with the Swifht/XRT telescope in April 2013. For several months after its detection the source was observed with the NuSTAR observatory, which allowed pulsations with a period $\sim3.76$ s to be recorded. Using these observations, we have studied in detail the dependence of the pulse profile and the pulsed fraction on the energy and intensity of the magnetar. The pulsed fraction in the 3-5 and 5-10 keV energy bands is shown to be 40-50%, slightly increasing with decreasing flux. We have performed phase-resolved spectroscopy for the source in the energy band from 3 to $\sim$40 keV and show that the temperature of the emitting regions remains fairly stable during the pulse, while their apparent size changes significantly with phase.