English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Observations of the fluorescent Fe K-alpha emission line from the inneraccretion flows of stellar mass black holes in X-ray binaries and supermassiveblack holes in Active Galactic Nuclei have become an important tool to studythe magnitude and inclination of the black hole spin, and the structure of theaccretion flow close to the event horizon of the black hole. Modeling spectral,timing, and soon also X-ray polarimetric observations of the Fe K-alphaemission requires to calculate the specific intensity in the rest frame of theemitting plasma. We revisit the derivation of the equation used for calculatingthe illumination of the accretion disk by the corona. We present an alternativederivation leading to a simpler equation, and discuss the relation to thepreviously published results.

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