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Phase-resolved spectral analysis of the 11 mHz quasi-periodic oscillation in the black hole candidate H1743-322

Phase-resolved spectral analysis of the 11 mHz quasi-periodic oscillation in the black hole candidate H1743-322
Phase-resolved spectral analysis of the 11 mHz quasi-periodic oscillation in the black hole candidate H1743-322

H1743-322 is one of the few black hole candidates (BHCs) in low-mass X-ray binaries that shows mHz quasi-periodic oscillations (QPOs) that are not associated with the more common type A, B, and C oscillations seen in the X-ray light curves of typical BHC systems. To better understand the physical origin of the mHz oscillations, we carried out a phase-resolved spectroscopic study of two RXTE observations of this source. As previously reported, the averaged energy spectra of H1743-322 show a strong iron line at ~6.5 keV. Here we found evidence that the line flux appears to be modulated at twice the frequency of the mHz QPO. This line flux modulation is very similar to the one previously found for the type-C QPO in this source. We interpret the possibly periodic line flux modulation with this mHz QPO in terms of Lense-Thirring precession of the inner flow, and discuss the possible connection with the modulation of the line properties with the type-C QPO frequency.

Accretion, Accretion discs, Black hole physics, Relativistic processes, X-rays: individual: H1743-322
0035-8711
550-559
Cheng, Zheng
150adaed-6ec2-4476-8896-8b38ea2a3cda
Méndez, Mariano
5cc6f759-dae2-488a-9cc2-cff89f4eca72
Altamirano, Diego
d5ccdb09-0b71-4303-9538-05b467be075b
Beri, Aru
69ed346a-f02a-4243-83f9-ad5ab4c4008c
Wang, Yanan
37b2021a-5d54-4360-ace2-4fc34e69ee90
Cheng, Zheng
150adaed-6ec2-4476-8896-8b38ea2a3cda
Méndez, Mariano
5cc6f759-dae2-488a-9cc2-cff89f4eca72
Altamirano, Diego
d5ccdb09-0b71-4303-9538-05b467be075b
Beri, Aru
69ed346a-f02a-4243-83f9-ad5ab4c4008c
Wang, Yanan
37b2021a-5d54-4360-ace2-4fc34e69ee90

Cheng, Zheng, Méndez, Mariano, Altamirano, Diego, Beri, Aru and Wang, Yanan (2019) Phase-resolved spectral analysis of the 11 mHz quasi-periodic oscillation in the black hole candidate H1743-322. Monthly Notices of the Royal Astronomical Society, 482 (1), 550-559. (doi:10.1093/mnras/sty2695).

Record type: Article

Abstract

H1743-322 is one of the few black hole candidates (BHCs) in low-mass X-ray binaries that shows mHz quasi-periodic oscillations (QPOs) that are not associated with the more common type A, B, and C oscillations seen in the X-ray light curves of typical BHC systems. To better understand the physical origin of the mHz oscillations, we carried out a phase-resolved spectroscopic study of two RXTE observations of this source. As previously reported, the averaged energy spectra of H1743-322 show a strong iron line at ~6.5 keV. Here we found evidence that the line flux appears to be modulated at twice the frequency of the mHz QPO. This line flux modulation is very similar to the one previously found for the type-C QPO in this source. We interpret the possibly periodic line flux modulation with this mHz QPO in terms of Lense-Thirring precession of the inner flow, and discuss the possible connection with the modulation of the line properties with the type-C QPO frequency.

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Accepted/In Press date: 1 October 2018
e-pub ahead of print date: 4 October 2018
Published date: 1 January 2019
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Keywords: Accretion, Accretion discs, Black hole physics, Relativistic processes, X-rays: individual: H1743-322

Identifiers

Local EPrints ID: 427185
URI: http://eprints.soton.ac.uk/id/eprint/427185
ISSN: 0035-8711
PURE UUID: e8fc696a-4e2d-41f7-8742-7bf07da32239
ORCID for Diego Altamirano: ORCID iD orcid.org/0000-0002-3422-0074

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Date deposited: 04 Jan 2019 17:30
Last modified: 07 Oct 2020 02:05

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Contributors

Author: Zheng Cheng
Author: Mariano Méndez
Author: Aru Beri
Author: Yanan Wang

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