Hostname: page-component-78c5997874-s2hrs Total loading time: 0 Render date: 2024-11-02T21:15:40.929Z Has data issue: false hasContentIssue false
  • English
  • Français

Probing accretion flow structure of the HMXB Centaurus X-3 through X-ray spectral variability

Published online by Cambridge University Press:  27 February 2023

Tsubasa Tamba Open the ORCID record for Tsubasa Tamba [Opens in a new window] ,
Hirokazu Odaka ,
Aya Bamba ,
Atsushi Tanimoto ,
Satoshi Takashima  and
Hiromasa Suzuki
Tsubasa Tamba
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected]
Hirokazu Odaka
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected] Kavli IPMU (WPI), UTIAS, The University of Tokyo, 5-1-5 Kashiwanoha, Chiba, Japan Research Center for the Early Universe, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan
Aya Bamba
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected] Kavli IPMU (WPI), UTIAS, The University of Tokyo, 5-1-5 Kashiwanoha, Chiba, Japan
Atsushi Tanimoto
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected]
Satoshi Takashima
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, Japan email: [email protected]
Hiromasa Suzuki
Affiliation:
Department of Physics, Konan University, 8-9-1 Okamoto, Higashinada-ku, Kobe, Hyogo, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We analyzed 39 ks NuSTAR data of Cen X-3 through both orbital- and pulse-phase resolved spectroscopy. Orbital-phase resolved spectra show extrinsic fluctuations due to absorption by surrounding plasma, as the spectral fluctuation mainly emerges below 10 keV. Pulse-phase resolved spectra, on the other hand, show intrinsic fluctuations depending on effectiveness of Comptonization, since the spectrum becomes hard above 10 keV at the pulse peak.

Keywords

accretionaccretion disksstars: neutronX-rays: individual (Cen X-3)
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 335 - 337
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Becker, P. A., & Wolff, M. T. 2005, ApJL, 621, L45 CrossRefGoogle Scholar
Becker, P. A., & Wolff, M. T. 2007, ApJ, 654, 435 CrossRefGoogle Scholar
Santangelo, A., del Sordo, S., Segreto, A., et al. 1998, A&A, 340, L55 Google Scholar
Suchy, S., Pottschmidt, K., Wilms, J., et al. 2008, ApJ, 675, 1487 CrossRefGoogle Scholar