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Probing the Cyclotron line characteristics of 4U 1538-522 using AstroSat-LAXPC
Raman Res Inst, Dept Astron & Astrophys, Bangalore 560080, India.
Max Planck Inst Extraterr Phys, D-85748 Garching, Germany..
Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.;St Josephs Coll, Darjeeling 734104, India..
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
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2019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 484, no 1, p. L1-L6Article in journal (Refereed) Published
Abstract [en]

We report the first report on cyclotron line studies with the LAXPC instrument onboard AstroSat of the high-mass X-ray binary pulsar 4U 1538-52. During the observation of source that spanned about 1 d with a net exposure of 50 ks, the source X-ray flux remained constant. Pulse profile is double peaked in low-energy range and has a single peak in high-energy range, the transition taking place around the cyclotron line energy of the source. Cyclotron scattering feature (CRSF) is detected at similar to 22 keV with a very high significance in phase averaged spectrum, It is one of the highest signal to noise ratio detections of CRSF for this source. We performed detailed pulse-phase-resolved spectral analysis with 10 independent phase bins. We report the results of pulse-phase-resolved spectroscopy of the continuum and CRSF parameters. The cyclotron line parameters show pulse phase dependence over the entire phase with a CRSF energy variation of similar to 13 per cent, which is in agreement with previous studies, We also confirm the increase ill the centroid energy of the CRSF observed between the 1996-2004 (RXTE) and the 2012 (Suzaku) observations, reinforcing that the increase was a long-term change.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS , 2019. Vol. 484, no 1, p. L1-L6
Keywords [en]
binaries general, radiation mechanism non-thermal, (stars.) pulsars general, (stars:) pulsars individual 4U 1538-522, X-rays stars
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Astronomy, Astrophysics and Cosmology
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URN: urn:nbn:se:kth:diva-257828DOI: 10.1093/mnrasl/sly234ISI: 000482180300001OAI: oai:DiVA.org:kth-257828DiVA, id: diva2:1348957
Note

QC 20190906

Available from: 2019-09-06 Created: 2019-09-06 Last updated: 2019-09-06Bibliographically approved

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Raichur, Harsha

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