Phase-Resolved Spectroscopy of the Magnetar SGR J1745-2900 Based on Data from the NuSTAR Observatory. (arXiv:2106.05070v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kuznetsova_E/0/1/0/all/0/1">E. A. Kuznetsova</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Lutovinov_A/0/1/0/all/0/1">A. A. Lutovinov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Semena_A/0/1/0/all/0/1">A. N. Semena</a> (1) ((1) Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117997, Russia)
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$40 keV and show that the temperature of the
emitting regions remains fairly stable during the pulse, while their apparent
size changes significantly with phase.
The magnetar SGR J1745-2900 located in the vicinity of the supermassive black
hole Sgr A$^{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.
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