Simulations and Analysis of Gravitationally Redshifted Kerr Black Hole Accretion Discs | Zendy

Benjamin Puzantian | Zendy; Steve Desjardins | Zendy; Christian Gigualt | Zendy

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Simulations and Analysis of Gravitationally Redshifted Kerr Black Hole Accretion Discs

Author(s) -

Benjamin Puzantian,

Steve Desjardins,

Christian Gigualt

Publication year - 2019

Publication title -

journal of undergraduate reports in physics

Language(s) - English

Resource type - Journals

ISSN - 2642-7451

DOI - 10.1063/1.5129247

Subject(s) - physics , kerr metric , astrophysics , rotating black hole , angular momentum , accretion (finance) , supermassive black hole , black hole (networking) , galaxy , binary black hole , fourier transform , redshift , classical mechanics , schwarzschild radius , gravitational wave , quantum mechanics , computer network , routing protocol , routing (electronic design automation) , computer science , link state routing protocol

The Kerr black hole rotates with two parameters: mass M and angular momentum a and is characterized by the Kerr metric (Taylor and Wheeler 2000). Hence, a binary pair of a black hole and a star can create an accretion disc. A Kerr ray tracer algorithm was used to simulate accretion discs in the Seyfert-1 galaxy. The power law observed flux of relativistic emission lines, and Kerr Fourier image analysis methods were applied to the simulated discs. Simulated image characteristics were analyzed. Power laws were fitted to the simulated data of the Mrk110 accretion disc. Lastly, the simulated images were transformed into Fourier space and characteristics were discussed.

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