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A two-component Comptonisation model for the type-B QPO in MAXI J1348-630

A two-component Comptonisation model for the type-B QPO in MAXI J1348-630
A two-component Comptonisation model for the type-B QPO in MAXI J1348-630

Spectral-timing analysis of the fast variability observed in X-rays is a powerful tool to study the physical and geometrical properties of the accretion/ejection flows in black hole (BH) binaries. The origin of type-B quasi-periodic oscillations (QPO), predominantly observed in BH candidates in the soft-intermediate state, has been linked to emission arising from the relativistic jet. In this state, the X-ray spectrum is characterized by a soft-thermal blackbody-like emission due to the accretion disc, an iron emission line (in the 6-7 keV range), and a power-law-like hard component due to inverse-Compton scattering of the soft-photon source by hot electrons in a corona or the relativistic jet itself. The spectral-timing properties of MAXI J1348-630 have been recently studied using observations obtained with the NICER observatory. The data show a strong type-B QPO at ∼4.5 Hz with increasing fractional rms amplitude with energy and positive lags with respect to a reference band at 2-2.5 keV. We use a variable-Comptonization model that assumes a sinusoidal coherent oscillation of the Comptonized X-ray flux and the physical parameters of the corona at the QPO frequency, to fit simultaneously the energy-dependent fractional rms amplitude and phase lags of this QPO. We show that two physically connected Comptonization regions can successfully explain the radiative properties of the QPO in the full 0.8-10 keV energy range.

X-rays: Binaries, X-rays: Individual (MAXI J1348-630), accretion, accretion discs, black hole physics, stars: Black holes
3173–3182
García, Federico
7c0fed66-dda4-4333-b38c-175f570820ce
Méndez, Mariano
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Karpouzas, Konstantinos
d796fbbc-2dbb-4244-8c06-ad6466a9abc0
Belloni, Tomaso
55fb4c9b-fe03-4af0-bd02-201635b1ea20
Zhang, Liang
77199a72-9bb0-4336-bbff-15c8e1b790cb
Altamirano, Diego
d5ccdb09-0b71-4303-9538-05b467be075b
García, Federico
7c0fed66-dda4-4333-b38c-175f570820ce
Méndez, Mariano
5cc6f759-dae2-488a-9cc2-cff89f4eca72
Karpouzas, Konstantinos
d796fbbc-2dbb-4244-8c06-ad6466a9abc0
Belloni, Tomaso
55fb4c9b-fe03-4af0-bd02-201635b1ea20
Zhang, Liang
77199a72-9bb0-4336-bbff-15c8e1b790cb
Altamirano, Diego
d5ccdb09-0b71-4303-9538-05b467be075b

García, Federico, Méndez, Mariano, Karpouzas, Konstantinos, Belloni, Tomaso, Zhang, Liang and Altamirano, Diego (2021) A two-component Comptonisation model for the type-B QPO in MAXI J1348-630. Monthly Notices of the Royal Astronomical Society, 501 (3), 3173–3182. (doi:10.1093/mnras/staa3944).

Record type: Article

Abstract

Spectral-timing analysis of the fast variability observed in X-rays is a powerful tool to study the physical and geometrical properties of the accretion/ejection flows in black hole (BH) binaries. The origin of type-B quasi-periodic oscillations (QPO), predominantly observed in BH candidates in the soft-intermediate state, has been linked to emission arising from the relativistic jet. In this state, the X-ray spectrum is characterized by a soft-thermal blackbody-like emission due to the accretion disc, an iron emission line (in the 6-7 keV range), and a power-law-like hard component due to inverse-Compton scattering of the soft-photon source by hot electrons in a corona or the relativistic jet itself. The spectral-timing properties of MAXI J1348-630 have been recently studied using observations obtained with the NICER observatory. The data show a strong type-B QPO at ∼4.5 Hz with increasing fractional rms amplitude with energy and positive lags with respect to a reference band at 2-2.5 keV. We use a variable-Comptonization model that assumes a sinusoidal coherent oscillation of the Comptonized X-ray flux and the physical parameters of the corona at the QPO frequency, to fit simultaneously the energy-dependent fractional rms amplitude and phase lags of this QPO. We show that two physically connected Comptonization regions can successfully explain the radiative properties of the QPO in the full 0.8-10 keV energy range.

Text
2012.10354v1 - Accepted Manuscript
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More information

Accepted/In Press date: 18 December 2020
e-pub ahead of print date: 26 December 2020
Published date: 1 March 2021
Additional Information: 11 pages, 6 figures, 3 tables. Accepted for publication in MNRAS
Keywords: X-rays: Binaries, X-rays: Individual (MAXI J1348-630), accretion, accretion discs, black hole physics, stars: Black holes

Identifiers

Local EPrints ID: 447642
URI: http://eprints.soton.ac.uk/id/eprint/447642
PURE UUID: a11a30e5-9d3b-4d85-bacc-62355da21e87
ORCID for Diego Altamirano: ORCID iD orcid.org/0000-0002-3422-0074

Catalogue record

Date deposited: 17 Mar 2021 17:35
Last modified: 26 Nov 2021 03:02

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Contributors

Author: Federico García
Author: Mariano Méndez
Author: Tomaso Belloni
Author: Liang Zhang

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