Study of the X-ray Pulsar XTE J1946+274 with NuSTAR View Full Text


Ontology type: schema:ScholarlyArticle      Open Access: True


Article Info

DATE

2021-06

AUTHORS

A. S. Gorban, S. V. Molkov, S. S. Tsygankov, A. A. Lutovinov

ABSTRACT

We present the results of our spectral and timing analysis of the emission from the transient X-ray pulsar XTE J1946+274 based on the simultaneous NuSTAR and Swift/XRT observations in the broad energy range 0.3–79 keV carried out in June 2018 during a bright outburst. Our spectral analysis has confirmed the presence of a cyclotron absorption line at an energy \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$${\sim}38$$\end{document} keV in both averaged and phase-resolved spectra of the source. Phase-resolved spectroscopy has also allowed the variation in spectral parameters with neutron star rotation phase, whose period is \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$${\simeq}15.755$$\end{document} s, to be studied. The energy of the cyclotron line is shown to change significantly (from \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$${\simeq}34$$\end{document} to \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$${\simeq}39$$\end{document} keV) on the scale of a pulse, with the line width and optical depth also exhibiting variability. The observed behavior of the cyclotron line parameters can be interpreted in terms of the model of the reflection of emission from a small accretion column (the source’s luminosity at the time of its observations was \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$${\sim}3\times 10^{37}$$\end{document} erg s\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$${}^{-1}$$\end{document}) off the neutron star surface. The equivalent width of the iron line has been found to also change significantly with pulse phase. The time delay between the pulse and equivalent width profiles can be explained by the reflection of neutron star emission from the outer accretion disk regions. More... »

PAGES

390-401

Identifiers

URI

http://scigraph.springernature.com/pub.10.1134/s1063773721060049

DOI

http://dx.doi.org/10.1134/s1063773721060049

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1142131148


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168 Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, 117997, Moscow, Russia
169 rdf:type schema:Organization
170 grid-institutes:grid.426428.e schema:alternateName Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, 117997, Moscow, Russia
171 schema:name Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, 117997, Moscow, Russia
172 Tuorla Observatory, University of Turku, Turku, Finland
173 rdf:type schema:Organization
 




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