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Constraining the mass of the black hole GX 339-4 using spectro-temporal analysis of multiple outbursts
URSC, Space Astron Grp, ISITE Campus,Outer Ring Rd, Bangalore 560037, Karnataka, India.;Indian Inst Sci, Bangalore 560012, Karnataka, India..
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
Dayananda Sagar Univ, Dept Phys, Bangalore 560068, Karnataka, India..
URSC, Space Astron Grp, ISITE Campus,Outer Ring Rd, Bangalore 560037, Karnataka, India..
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2019 (English)In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 63, no 3, p. 1374-1386Article in journal (Refereed) Published
Abstract [en]

We carried out spectro-temporal analysis of the archived data from multiple outbursts spanning over the last two decades from the black hole X-ray binary GX 339-4. In this paper, the mass of the compact object in the X-ray binary system GX 339-4 is constrained based on three indirect methods. The first method uses broadband spectral modelling with a two component flow structure of the accretion around the black hole. The broadband data are obtained from RXTE (Rossi X-ray Timing Explorer) in the range 3.0 to 150.0 keV and from Swift and NuSTAR (Nuclear Spectroscopic Telescope Array) simultaneously in the range 0.5 to 79.0 keV. In the second method, we model the time evolution of Quasi-periodic Oscillation (QPO) frequencies, considering it to be the result of an oscillating shock that radially propagates towards or away from the compact object. The third method is based on scaling a mass dependent parameter from an empirical model of the photon index (Gamma) - QPO (v) correlation. We compare the results at 90 percent confidence from the three methods and summarize the mass estimate of the central object to be in the range 8.28-11.89M(circle dot). 

Place, publisher, year, edition, pages
ELSEVIER SCI LTD , 2019. Vol. 63, no 3, p. 1374-1386
Keywords [en]
Black hole candidate, Accretion discs, X ray outbursts
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:kth:diva-244527DOI: 10.1016/j.asr.2018.10.042ISI: 000457951400020Scopus ID: 2-s2.0-85056391444OAI: oai:DiVA.org:kth-244527DiVA, id: diva2:1302125
Note

QC 20190403

Available from: 2019-04-03 Created: 2019-04-03 Last updated: 2019-04-04Bibliographically approved

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