Normalizing a relativistic model of X-ray reflection
Thomas DauserRemeis Observatory & ECAP, Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, GermanyJavier A. GarcíaHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAD. J. WaltonCahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAW. EikmannRemeis Observatory & ECAP, Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, GermanyT. R. KallmanX-ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USAJ. E. McClintockHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAJ. WilmsRemeis Observatory & ECAP, Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany
2016en
ABI
Annotatsiya
Aims. The only relativistic reflection model that implements a parameter relating the intensity incident on an accretion disk to the observed intensity is relxill. The parameter used in earlier versions of this model, referred to as the reflection strength, is unsatisfactory; it has been superseded by a parameter that provides insight into the accretion geometry, namely the reflection fraction. The reflection fraction is defined as the ratio of the coronal intensity illuminating the disk to the coronal intensity that reaches the observer.
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