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....
| Main Authors: | , , , , |
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| Format: | Journal article |
| Language: | English |
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Oxford University Press
2016
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| _version_ | 1826263350373253120 |
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| author | Ingram, A Van Der Klis, M Middleton, M Altamirano, D Uttley, P |
| author_facet | Ingram, A Van Der Klis, M Middleton, M Altamirano, D Uttley, P |
| author_sort | Ingram, A |
| collection | OXFORD |
| description | 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. |
| first_indexed | 2024-03-06T19:50:22Z |
| format | Journal article |
| id | oxford-uuid:23c210c4-06c6-4179-ba2e-654262b825b3 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T19:50:22Z |
| publishDate | 2016 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:23c210c4-06c6-4179-ba2e-654262b825b32022-03-26T11:46:01ZTomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743−322Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:23c210c4-06c6-4179-ba2e-654262b825b3EnglishSymplectic Elements at OxfordOxford University Press2016Ingram, AVan Der Klis, MMiddleton, MAltamirano, DUttley, PAccreting 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. |
| spellingShingle | Ingram, A Van Der Klis, M Middleton, M Altamirano, D Uttley, P Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743−322 |
| title | Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743−322 |
| title_full | Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743−322 |
| title_fullStr | Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743−322 |
| title_full_unstemmed | Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743−322 |
| title_short | Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743−322 |
| title_sort | tomographic reflection modelling of quasi periodic oscillations in the black hole binary h 1743 322 |
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