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Title: On the Calculation of the Fe K-alpha Line Emissivity of Black Hole Accretion Disks

Abstract

Observations of the fluorescent Fe K α emission line from the inner accretion flows of stellar mass black holes in X-ray binaries and supermassive black holes in active galactic nuclei have become an important tool to study the magnitude and inclination of the black hole spin, and the structure of the accretion flow close to the event horizon of the black hole. Modeling spectral, timing, and soon also X-ray polarimetric observations of the Fe K α emission requires the calculation of the specific intensity in the rest frame of the emitting plasma. We revisit the derivation of the equation used for calculating the illumination of the accretion disk by the corona. We present an alternative derivation leading to a simpler equation, and discuss the relation to previously published results.

Authors:
;  [1]
  1. Physics Department and McDonnell Center for the Space Sciences, Washington University in St. Louis, 1 Brookings Drive, CB 1105, St. Louis, MO 63130 (United States)
Publication Date:
OSTI Identifier:
22679707
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 849; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCRETION DISKS; BLACK HOLES; EMISSIVITY; FLUORESCENCE; GALAXY NUCLEI; ILLUMINANCE; INCLINATION; IRON; K ABSORPTION; MASS; PLASMA; QUASARS; SIMULATION; SUPERMASSIVE STARS; X RADIATION

Citation Formats

Krawczynski, H., and Beheshtipour, B., E-mail: krawcz@wustl.edu. On the Calculation of the Fe K-alpha Line Emissivity of Black Hole Accretion Disks. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA8DFF.
Krawczynski, H., & Beheshtipour, B., E-mail: krawcz@wustl.edu. On the Calculation of the Fe K-alpha Line Emissivity of Black Hole Accretion Disks. United States. doi:10.3847/1538-4357/AA8DFF.
Krawczynski, H., and Beheshtipour, B., E-mail: krawcz@wustl.edu. Wed . "On the Calculation of the Fe K-alpha Line Emissivity of Black Hole Accretion Disks". United States. doi:10.3847/1538-4357/AA8DFF.
@article{osti_22679707,
title = {On the Calculation of the Fe K-alpha Line Emissivity of Black Hole Accretion Disks},
author = {Krawczynski, H. and Beheshtipour, B., E-mail: krawcz@wustl.edu},
abstractNote = {Observations of the fluorescent Fe K α emission line from the inner accretion flows of stellar mass black holes in X-ray binaries and supermassive black holes in active galactic nuclei have become an important tool to study the magnitude and inclination of the black hole spin, and the structure of the accretion flow close to the event horizon of the black hole. Modeling spectral, timing, and soon also X-ray polarimetric observations of the Fe K α emission requires the calculation of the specific intensity in the rest frame of the emitting plasma. We revisit the derivation of the equation used for calculating the illumination of the accretion disk by the corona. We present an alternative derivation leading to a simpler equation, and discuss the relation to previously published results.},
doi = {10.3847/1538-4357/AA8DFF},
journal = {Astrophysical Journal},
number = 1,
volume = 849,
place = {United States},
year = {Wed Nov 01 00:00:00 EDT 2017},
month = {Wed Nov 01 00:00:00 EDT 2017}
}