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Irradiation of an accretion disc by a jet: general properties and implications for spin measurements of black holes

Thomas DauserDr Karl Remeis-Observatory and Erlangen Centre for Astroparticle Physics, Sternwartstr. 7, D-96049 Bamberg, GermanyJavier A. GarcíaDepartment of Astronomy and Maryland Astronomy Center for Theory and Computation, University of Maryland, College Park, MD 20742, USAJ. WilmsDr Karl Remeis-Observatory and Erlangen Centre for Astroparticle Physics, Sternwartstr. 7, D-96049 Bamberg, GermanyM. BöckMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyLaura BrennemanHarvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAM. FalangaInternational Space Science Institute, Hallerstrasse 6, CH-3012 Bern, SwitzerlandKeigo FukumuraAstrophysics Science Division, NASA Goddard Space Flight Center, Code 663, Greenbelt, MD 20771, USAC. S. ReynoldsDepartment of Astronomy and Maryland Astronomy Center for Theory and Computation, University of Maryland, College Park, MD 20742, USA

2013en

ABI

Annotatsiya

X-ray irradiation of the accretion disc leads to strong reflection features, which are then broadened and distorted by relativistic effects. We present a detailed, general relativistic approach to model this irradiation for different geometries of the primary X-ray source. These geometries include the standard point source on the rotational axis as well as more jet-like sources, which are radially elongated and accelerating. Incorporating this code in the relline model for relativistic line emission, the line shape for any configuration can be predicted. We study how different irradiation geometries affect the determination of the spin of the black hole. Broad emission lines are produced only for compact irradiating sources situated close to the black hole. This is the only case where the black hole spin can be unambiguously determined. In all other cases the line shape is narrower, which could either be explained by a low spin or an elongated source. We conclude that for all those cases and independent of the quality of the data, no unique solution for the spin exists and therefore only a lower limit of the spin value can be given.

Identifikatorlar

DOI: 10.1093/mnras/sts710

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