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Investigating the timing and spectral signatures of Be/X-ray pulsar RX J0520.5−6932 during its 2024 outburst using NuSTAR.

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Title: Investigating the timing and spectral signatures of Be/X-ray pulsar RX J0520.5−6932 during its 2024 outburst using NuSTAR.
Authors: Jain, Chetana1 (AUTHOR) chetanajain11@gmail.com
Source: Journal of Astrophysics & Astronomy. 5/21/2025, Vol. 46 Issue 1, p1-12. 12p.
Subjects: Large Magellanic Cloud, Binary pulsars, Magnetic flux density, X-ray binaries, Physical sciences
Abstract: The Be X-ray binary pulsar RX J0520.5 - 6932 in the Large Magellanic Cloud recently underwent an outburst after a gap of about 10 years. This paper presents the timing and spectral analysis of this transient system using the NuSTAR observation that was made near the peak of the outburst. Coherent pulsations were detected with a period of 8.029877(9) s (at MJD 60412.87) up to 50 keV. The pulse profile was single-peaked and asymmetric, with the presence of two local minima on the slowly rising edge up to about 18 keV. The hard X-ray pulse profiles were relatively smooth. The 3–50 keV FPMA–FPMB energy spectrum was well described by a thermally comptonized continuum with an electron temperature of ∼ 5.3 keV and a photon index of ∼ 1.36. A broad ∼ 6.32 keV Fe emission line and a cyclotron resonant scattering feature (CRSF) with ∼ 32.3 keV central energy, corresponding to a surface magnetic field strength of ∼ 2.8 × 10 12 G were also required to describe the energy spectrum. The pulse phase resolved spectroscopy indicated significant variation in energy and width of the CRSF and iron emission line. A ∼ 14.6 keV absorption feature was also detected at specific pulse phases. [ABSTRACT FROM AUTHOR]
Copyright of Journal of Astrophysics & Astronomy is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Investigating the timing and spectral signatures of Be/X-ray pulsar RX J0520.5−6932 during its 2024 outburst using NuSTAR.
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  Data: <searchLink fieldCode="AR" term="%22Jain%2C+Chetana%22">Jain, Chetana</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> chetanajain11@gmail.com</i>
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Astrophysics+%26+Astronomy%22">Journal of Astrophysics & Astronomy</searchLink>. 5/21/2025, Vol. 46 Issue 1, p1-12. 12p.
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  Data: <searchLink fieldCode="DE" term="%22Large+Magellanic+Cloud%22">Large Magellanic Cloud</searchLink><br /><searchLink fieldCode="DE" term="%22Binary+pulsars%22">Binary pulsars</searchLink><br /><searchLink fieldCode="DE" term="%22Magnetic+flux+density%22">Magnetic flux density</searchLink><br /><searchLink fieldCode="DE" term="%22X-ray+binaries%22">X-ray binaries</searchLink><br /><searchLink fieldCode="DE" term="%22Physical+sciences%22">Physical sciences</searchLink>
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  Label: Abstract
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  Data: The Be X-ray binary pulsar RX J0520.5 - 6932 in the Large Magellanic Cloud recently underwent an outburst after a gap of about 10 years. This paper presents the timing and spectral analysis of this transient system using the NuSTAR observation that was made near the peak of the outburst. Coherent pulsations were detected with a period of 8.029877(9) s (at MJD 60412.87) up to 50 keV. The pulse profile was single-peaked and asymmetric, with the presence of two local minima on the slowly rising edge up to about 18 keV. The hard X-ray pulse profiles were relatively smooth. The 3–50 keV FPMA–FPMB energy spectrum was well described by a thermally comptonized continuum with an electron temperature of ∼ 5.3 keV and a photon index of ∼ 1.36. A broad ∼ 6.32 keV Fe emission line and a cyclotron resonant scattering feature (CRSF) with ∼ 32.3 keV central energy, corresponding to a surface magnetic field strength of ∼ 2.8 × 10 12 G were also required to describe the energy spectrum. The pulse phase resolved spectroscopy indicated significant variation in energy and width of the CRSF and iron emission line. A ∼ 14.6 keV absorption feature was also detected at specific pulse phases. [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
  Label:
  Group: Ab
  Data: <i>Copyright of Journal of Astrophysics & Astronomy is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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        Value: 10.1007/s12036-025-10057-9
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        Type: general
      – SubjectFull: Binary pulsars
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      – SubjectFull: Magnetic flux density
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              Text: 5/21/2025
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