NuSTAR view of Be/X-ray binary pulsar 2S 1417?624 during 2018 giant outburst

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dc.contributor.author Gupta, Shivangi
dc.contributor.author Naik, Sachindra
dc.contributor.author Jaisawal, Gaurava K.
dc.date.accessioned 2020-03-12T08:51:46Z
dc.date.available 2020-03-12T08:51:46Z
dc.date.issued 2019-12
dc.identifier.citation Gupta, Shivangi; Naik, Sachindra and Jaisawal, Gaurava K. "NuSTAR view of Be/X-ray binary pulsar 2S 1417?624 during 2018 giant outburst", Monthly Notices of the Royal Astronomical Society, DOI: 10.1093/mnras/stz2795, vol. 490, no. 2, pp. 2458-2466, Dec. 2019. en_US
dc.identifier.issn 0035-8711
dc.identifier.issn 1365-2966
dc.identifier.uri https://doi.org/10.1093/mnras/stz2795
dc.identifier.uri https://repository.iitgn.ac.in/handle/123456789/5225
dc.description.abstract We report the results obtained from a detailed timing and spectral studies of Be/X-ray binary pulsar 2S 1417?624 using data from Swift and NuSTAR observatories. The observations were carried out at the peak of a giant outburst of the pulsar in 2018. X-ray pulsations at ?17.475 s were detected in the source light curves up to 79 keV. The evolution of the pulse profiles with energy was found to be complex. A four-peaked profile at lower energies gradually evolved into a double-peak structure at higher energies. The pulsed fraction of the pulsar, calculated from the NuSTAR observation was found to follow an anticorrelation trend with luminosity as observed during previous giant X-ray outburst studies in 2009. The broad-band spectrum of the pulsar is well described by a composite model consisting of a cut-off power-law model modified with the interstellar absorption, a thermal blackbody component with a temperature of ?1 keV, and a Gaussian function for the 6.4 keV iron emission line. Though the pulsar was observed at the peak of the giant outburst, there was no signature of presence of any cyclotron line feature in the spectrum. The radius of the blackbody emitting region was estimated to be ?2 km, suggesting that the most probable site of its origin is the stellar surface of the neutron star. Physical models were also explored to understand the emission geometry of the pulsar and are discussed in the paper.
dc.description.statementofresponsibility by Shivangi Gupta, Sachindra Naik and Gaurava K Jaisawa
dc.format.extent vol. 490, no. 2, pp. 2458-2466
dc.language.iso en_US en_US
dc.publisher Oxford University Press en_US
dc.subject stars: magnetic field en_US
dc.subject stars: neutron en_US
dc.subject pulsars: individual: 2S 1417-624 en_US
dc.subject X-rays: binaries en_US
dc.subject X-rays: stars en_US
dc.title NuSTAR view of Be/X-ray binary pulsar 2S 1417?624 during 2018 giant outburst en_US
dc.type Article en_US
dc.relation.journal Monthly Notices of the Royal Astronomical Society


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