High energy radiation from jets and accretion disks near rotating black holes

Michael O'Riordan; Asaf Pe'Er; Jonathan C. McKinney

doi:10.1063/1.4968946

High energy radiation from jets and accretion disks near rotating black holes

Michael O'Riordan, Asaf Pe'Er, Jonathan C. McKinney

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review

Abstract

We model the low/hard state in X-ray binaries as a magnetically arrested accretion flow, and calculate the resulting radiation using a general-relativistic radiative transport code. Firstly, we investigate the origin of the high-energy emission. We find the following indications of a significant jet contribution at high energies: (i) a pronounced γ-ray peak at ∼ 10²³ Hz, (ii) a break in the optical/UV band where the spectrum changes from disk to jet dominated, and (iii) a low-frequency synchrotron peak ≲ 10¹⁴ Hz implies that a significant fraction of any observed X-ray and γ-ray emission originates in the jet. Secondly, we investigate the effects of black hole spin on the high-energy emission. We find that the X-ray and γ-ray power depend strongly on spin and inclination angle. Surprisingly, this dependence is not a result of the Blandford-Znajek mechanism, but instead can be understood as a redshift effect. For rapidly rotating black holes, observers with large inclinations see deeper into the hot, dense, highly-magnetized inner regions of the accretion flow. Since the lower frequency emission originates at larger radii, it is not significantly affected by the spin. Therefore, the ratio of the X-ray to near-infrared power is an observational probe of black hole spin.

Original language	English
Title of host publication	High Energy Gamma-Ray Astronomy
Subtitle of host publication	6th International Meeting on High Energy Gamma-Ray Astronomy
Editors	Felix A. Aharonian, Felix A. Aharonian, Frank M. Rieger, Werner Hofmann
Publisher	American Institute of Physics Inc.
ISBN (Electronic)	9780735414563
DOIs	https://doi.org/10.1063/1.4968946
State	Published - 4 Jan 2017
Externally published	Yes
Event	6th International Symposium on High Energy Gamma-Ray Astronomy - Heidelberg, Germany Duration: 11 Jul 2016 → 15 Jul 2016

Publication series

Name	AIP Conference Proceedings
Volume	1792
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Conference

Conference	6th International Symposium on High Energy Gamma-Ray Astronomy
Country/Territory	Germany
City	Heidelberg
Period	11/07/16 → 15/07/16

Bibliographical note

Publisher Copyright:
© 2017 Author(s).

Funding

JCM would like to thank Alexander Tchekhovskoy for providing simulation data. MOR is supported by the Irish Research Council under grant number GOIPG/2013/315. This research was partially supported by the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no 618499. JCM acknowledges NASA/NSF/TCAN (NNX14AB46G), NSF/XSEDE/TACC (TGPHY120005), and NASA/Pleiades (SMD-14-5451).

Funders	Funder number
Pleiades	SMD-14-5451
TACC	TGPHY120005
TCAN	NNX14AB46G
XSEDE
National Science Foundation
National Aeronautics and Space Administration
Seventh Framework Programme	618499
Irish Research Council	GOIPG/2013/315
Seventh Framework Programme

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10.1063/1.4968946

Cite this

O'Riordan, M., Pe'Er, A., & McKinney, J. C. (2017). High energy radiation from jets and accretion disks near rotating black holes. In F. A. Aharonian, F. A. Aharonian, F. M. Rieger, & W. Hofmann (Eds.), High Energy Gamma-Ray Astronomy: 6th International Meeting on High Energy Gamma-Ray Astronomy Article 040042 (AIP Conference Proceedings; Vol. 1792). American Institute of Physics Inc.. https://doi.org/10.1063/1.4968946

O'Riordan, Michael ; Pe'Er, Asaf ; McKinney, Jonathan C. / High energy radiation from jets and accretion disks near rotating black holes. High Energy Gamma-Ray Astronomy: 6th International Meeting on High Energy Gamma-Ray Astronomy. editor / Felix A. Aharonian ; Felix A. Aharonian ; Frank M. Rieger ; Werner Hofmann. American Institute of Physics Inc., 2017. (AIP Conference Proceedings).

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abstract = "We model the low/hard state in X-ray binaries as a magnetically arrested accretion flow, and calculate the resulting radiation using a general-relativistic radiative transport code. Firstly, we investigate the origin of the high-energy emission. We find the following indications of a significant jet contribution at high energies: (i) a pronounced γ-ray peak at ∼ 1023 Hz, (ii) a break in the optical/UV band where the spectrum changes from disk to jet dominated, and (iii) a low-frequency synchrotron peak ≲ 1014 Hz implies that a significant fraction of any observed X-ray and γ-ray emission originates in the jet. Secondly, we investigate the effects of black hole spin on the high-energy emission. We find that the X-ray and γ-ray power depend strongly on spin and inclination angle. Surprisingly, this dependence is not a result of the Blandford-Znajek mechanism, but instead can be understood as a redshift effect. For rapidly rotating black holes, observers with large inclinations see deeper into the hot, dense, highly-magnetized inner regions of the accretion flow. Since the lower frequency emission originates at larger radii, it is not significantly affected by the spin. Therefore, the ratio of the X-ray to near-infrared power is an observational probe of black hole spin.",

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O'Riordan, M, Pe'Er, A & McKinney, JC 2017, High energy radiation from jets and accretion disks near rotating black holes. in FA Aharonian, FA Aharonian, FM Rieger & W Hofmann (eds), High Energy Gamma-Ray Astronomy: 6th International Meeting on High Energy Gamma-Ray Astronomy., 040042, AIP Conference Proceedings, vol. 1792, American Institute of Physics Inc., 6th International Symposium on High Energy Gamma-Ray Astronomy, Heidelberg, Germany, 11/07/16. https://doi.org/10.1063/1.4968946

High energy radiation from jets and accretion disks near rotating black holes. / O'Riordan, Michael; Pe'Er, Asaf; McKinney, Jonathan C.
High Energy Gamma-Ray Astronomy: 6th International Meeting on High Energy Gamma-Ray Astronomy. ed. / Felix A. Aharonian; Felix A. Aharonian; Frank M. Rieger; Werner Hofmann. American Institute of Physics Inc., 2017. 040042 (AIP Conference Proceedings; Vol. 1792).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review

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N2 - We model the low/hard state in X-ray binaries as a magnetically arrested accretion flow, and calculate the resulting radiation using a general-relativistic radiative transport code. Firstly, we investigate the origin of the high-energy emission. We find the following indications of a significant jet contribution at high energies: (i) a pronounced γ-ray peak at ∼ 1023 Hz, (ii) a break in the optical/UV band where the spectrum changes from disk to jet dominated, and (iii) a low-frequency synchrotron peak ≲ 1014 Hz implies that a significant fraction of any observed X-ray and γ-ray emission originates in the jet. Secondly, we investigate the effects of black hole spin on the high-energy emission. We find that the X-ray and γ-ray power depend strongly on spin and inclination angle. Surprisingly, this dependence is not a result of the Blandford-Znajek mechanism, but instead can be understood as a redshift effect. For rapidly rotating black holes, observers with large inclinations see deeper into the hot, dense, highly-magnetized inner regions of the accretion flow. Since the lower frequency emission originates at larger radii, it is not significantly affected by the spin. Therefore, the ratio of the X-ray to near-infrared power is an observational probe of black hole spin.

AB - We model the low/hard state in X-ray binaries as a magnetically arrested accretion flow, and calculate the resulting radiation using a general-relativistic radiative transport code. Firstly, we investigate the origin of the high-energy emission. We find the following indications of a significant jet contribution at high energies: (i) a pronounced γ-ray peak at ∼ 1023 Hz, (ii) a break in the optical/UV band where the spectrum changes from disk to jet dominated, and (iii) a low-frequency synchrotron peak ≲ 1014 Hz implies that a significant fraction of any observed X-ray and γ-ray emission originates in the jet. Secondly, we investigate the effects of black hole spin on the high-energy emission. We find that the X-ray and γ-ray power depend strongly on spin and inclination angle. Surprisingly, this dependence is not a result of the Blandford-Znajek mechanism, but instead can be understood as a redshift effect. For rapidly rotating black holes, observers with large inclinations see deeper into the hot, dense, highly-magnetized inner regions of the accretion flow. Since the lower frequency emission originates at larger radii, it is not significantly affected by the spin. Therefore, the ratio of the X-ray to near-infrared power is an observational probe of black hole spin.

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O'Riordan M, Pe'Er A, McKinney JC. High energy radiation from jets and accretion disks near rotating black holes. In Aharonian FA, Aharonian FA, Rieger FM, Hofmann W, editors, High Energy Gamma-Ray Astronomy: 6th International Meeting on High Energy Gamma-Ray Astronomy. American Institute of Physics Inc. 2017. 040042. (AIP Conference Proceedings). doi: 10.1063/1.4968946

High energy radiation from jets and accretion disks near rotating black holes

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