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Modelling the polarised emission from black holes on event horizon-scales

Published online by Cambridge University Press:  07 April 2020

Ziri Younsi ,
Oliver Porth ,
Yosuke Mizuno ,
Christian M. Fromm  and
Hector Olivares
Ziri Younsi
Affiliation:
Institut für Theoretische Physik, Max-von-Laue-Straße 1, D-60438 Frankfurt am Main, Germany email: younsi@itp.uni-frankfurt.de Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK email: z.younsi@ucl.ac.uk
Oliver Porth
Affiliation:
Institut für Theoretische Physik, Max-von-Laue-Straße 1, D-60438 Frankfurt am Main, Germany email: younsi@itp.uni-frankfurt.de
Yosuke Mizuno
Affiliation:
Institut für Theoretische Physik, Max-von-Laue-Straße 1, D-60438 Frankfurt am Main, Germany email: younsi@itp.uni-frankfurt.de
Christian M. Fromm
Affiliation:
Institut für Theoretische Physik, Max-von-Laue-Straße 1, D-60438 Frankfurt am Main, Germany email: younsi@itp.uni-frankfurt.de Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
Hector Olivares
Affiliation:
Institut für Theoretische Physik, Max-von-Laue-Straße 1, D-60438 Frankfurt am Main, Germany email: younsi@itp.uni-frankfurt.de
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Abstract

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Upcoming VLBI observations will resolve nearby supermassive black holes, most notably Sagittarius A* and M87, on event horizon-scales. Recent observations of Sagittarius A* with the Event Horizon Telescope have revealed horizon-scale structure. Accordingly, the detection and measurement of the back hole “shadow” is expected to enable the existence of astrophysical black holes to be verified directly. Although the theoretical description of the shadow is straightforward, its observational appearance is largely determined by the properties of the surrounding accretion flow, which is highly turbulent. We introduce a new polarised general-relativistic radiative transfer code, BHOSS, which accurately solves the equations of polarised radiative transfer in arbitrary strong-gravity environments, providing physically-realistic images of astrophysical black holes on event horizon-scales, as well as also providing insight into the fundamental properties and nature of the surrounding accretion flow environment.

Keywords

gravitationmethods: numericalradiative transferrelativitypolarisation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S342: Perseus in Sicily: From Black Hole to Cluster Outskirts , May 2018 , pp. 9 - 12
Copyright
© International Astronomical Union 2020

References

Doeleman, S. S., Weintroub, J., Rogers, A. E. E., Plambeck, R., et al. 2008, Nature, 78–80, 455Google Scholar
Goddi, C., Falcke, H., Kramer, M., et al. 2017, Int. J. Mod. Phys. D, 26, 1730001–239CrossRefGoogle Scholar
Cunningham, C. T. and Bardeen, J. M. 1973, Astrophys. J., 237–264, 183Google Scholar
Grenzebach, A., Perlick, V. and Lämmerzahl, C. 2014, Phys. Rev. D, 12, 89Google Scholar
Younsi, Z., Zhidenko, A., Rezzolla, L., Konoplya, R. & Mizuno, Y. 2016, Phys. Rev. D, 8, 94Google Scholar
Mizuno, Y., Younsi, Z., Fromm, C. M., Porth, O., De Laurentis, M., Olivares, H., Falcke, H., Kramer, M. & Rezzolla, L. 2018, Nature Astronomy, 2, 585–590CrossRefGoogle Scholar
Porth, O., Olivares, H., Mizuno, Y., Younsi, Z., Rezzolla, L.et al. 2017, CA&C, 1, 4Google Scholar
Gammie, C. F., McKinney, J. C. & Tóth, G. 2003, Astrophys. J., 458, 589Google Scholar
Teo, E. 2003 Gen. Rel. and Grav., 35, 11CrossRefGoogle Scholar
Chan, C.-k., Medeiros, L., Ozel, F. & Psaltis, D. 2017, ArXiv e-prints:1706.07062Google Scholar
Younsi, Z., Wu, K. and Fuerst, S. V. 2012, Astron. Astrophys., A13, 545Google Scholar
Broderick, A., & Blandford, R. 2003a, MNRAS, 342, 1280; 2003b, Ap&SS, 288, 161CrossRefGoogle Scholar
Shcherbakov, R. V. & Huang, L. 2011, MNRAS, 410, 1052CrossRefGoogle Scholar
Dexter, J. 2016, MNRAS, 462, 115CrossRefGoogle Scholar
Mościbrodzka, M. & Gammie, C. F. 2018, MNRAS, 475, 43–54CrossRefGoogle Scholar
Pihajoki, P., Mannerkoski, M., Nättilä, J. & Johansson, P. H. 2018, Astrophys. J., 863, 8CrossRefGoogle Scholar
Schnittman, J. D. & Krolik, J. H. 2010, Astrophys. J., 712, 908–924CrossRefGoogle Scholar
Dovčiak, M., Muleri, F., Goosmann, R. W., Karas, V. & Matt, G. 2008, MNRAS, 391, 32–38CrossRefGoogle Scholar