The University of Southampton
University of Southampton Institutional Repository

Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743–322

Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743–322
Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743–322
Accreting stellar mass black holes (BHs) routinely exhibit Type-C quasi-periodic oscillations (QPOs). These are often interpreted as Lense–Thirring precession of the inner accretion flow, a relativistic effect whereby the spin of the BH distorts the surrounding space–time, inducing nodal precession. The best evidence for the precession model is the recent discovery, using a long joint XMM–Newton and NuSTAR observation of H 1743−322, that the centroid energy of the iron florescence line changes systematically with QPO phase. This was interpreted as
the inner flow illuminating different azimuths of the accretion disc as it precesses, giving rise to a blueshifted/redshifted iron line when the approaching/receding disc material is illuminated. Here, we develop a physical model for this interpretation, including a self-consistent reflection continuum, and fit this to the same H 1743−322 data. We use an analytic function to parametrize the asymmetric illumination pattern on the disc surface that would result from inner flow precession, and find that the data are well described if two bright patches rotate about the disc surface. This model is preferred to alternatives considering an oscillating disc ionization parameter, disc inner radius and radial emissivity profile. We find that the reflection fraction varies with QPO phase (3.5σ), adding to the now formidable body of evidence that
Type-C QPOs are a geometric effect. This is the first example of tomographic QPO modelling, initiating a powerful new technique that utilizes QPOs in order to map the dynamics of accreting material close to the BH.
0035-8711
2979–2991
Ingram, Adam
01a02529-ad9f-4936-af5d-c200f88d4e53
van der Klis, Michiel
673255ce-dd17-4da0-910c-e3cb78460636
Middleton, Matthew
f91b89d9-fd2e-42ec-aa99-1249f08a52ad
Altamirano, Diego
d5ccdb09-0b71-4303-9538-05b467be075b
Uttley, Phil
db770bd7-d97e-43f5-99d4-a585bccd352a
Ingram, Adam
01a02529-ad9f-4936-af5d-c200f88d4e53
van der Klis, Michiel
673255ce-dd17-4da0-910c-e3cb78460636
Middleton, Matthew
f91b89d9-fd2e-42ec-aa99-1249f08a52ad
Altamirano, Diego
d5ccdb09-0b71-4303-9538-05b467be075b
Uttley, Phil
db770bd7-d97e-43f5-99d4-a585bccd352a

Ingram, Adam, van der Klis, Michiel, Middleton, Matthew, Altamirano, Diego and Uttley, Phil (2017) Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743–322. Monthly Notices of the Royal Astronomical Society, 464 (3), 2979–2991. (doi:10.1093/mnras/stw2581).

Record type: Article

Abstract

Accreting stellar mass black holes (BHs) routinely exhibit Type-C quasi-periodic oscillations (QPOs). These are often interpreted as Lense–Thirring precession of the inner accretion flow, a relativistic effect whereby the spin of the BH distorts the surrounding space–time, inducing nodal precession. The best evidence for the precession model is the recent discovery, using a long joint XMM–Newton and NuSTAR observation of H 1743−322, that the centroid energy of the iron florescence line changes systematically with QPO phase. This was interpreted as
the inner flow illuminating different azimuths of the accretion disc as it precesses, giving rise to a blueshifted/redshifted iron line when the approaching/receding disc material is illuminated. Here, we develop a physical model for this interpretation, including a self-consistent reflection continuum, and fit this to the same H 1743−322 data. We use an analytic function to parametrize the asymmetric illumination pattern on the disc surface that would result from inner flow precession, and find that the data are well described if two bright patches rotate about the disc surface. This model is preferred to alternatives considering an oscillating disc ionization parameter, disc inner radius and radial emissivity profile. We find that the reflection fraction varies with QPO phase (3.5σ), adding to the now formidable body of evidence that
Type-C QPOs are a geometric effect. This is the first example of tomographic QPO modelling, initiating a powerful new technique that utilizes QPOs in order to map the dynamics of accreting material close to the BH.

Text
__filestore.soton.ac.uk_users_jao1d15_mydocuments_ePrints_Diego.pdf - Accepted Manuscript
Download (755kB)

More information

Accepted/In Press date: 4 October 2016
e-pub ahead of print date: 8 October 2016
Published date: 21 January 2017
Organisations: Astronomy Group

Identifiers

Local EPrints ID: 401479
URI: http://eprints.soton.ac.uk/id/eprint/401479
ISSN: 0035-8711
PURE UUID: c1ff2869-2f8d-440d-a1e3-3d16b40ad792
ORCID for Diego Altamirano: ORCID iD orcid.org/0000-0002-3422-0074

Catalogue record

Date deposited: 17 Oct 2016 15:23
Last modified: 07 Oct 2020 05:27

Export record

Altmetrics

Contributors

Author: Adam Ingram
Author: Michiel van der Klis
Author: Phil Uttley

University divisions

Download statistics

Downloads from ePrints over the past year. Other digital versions may also be available to download e.g. from the publisher's website.

View more statistics

Atom RSS 1.0 RSS 2.0

Contact ePrints Soton: eprints@soton.ac.uk

ePrints Soton supports OAI 2.0 with a base URL of http://eprints.soton.ac.uk/cgi/oai2

This repository has been built using EPrints software, developed at the University of Southampton, but available to everyone to use.

We use cookies to ensure that we give you the best experience on our website. If you continue without changing your settings, we will assume that you are happy to receive cookies on the University of Southampton website.

×