Ray-tracing in pseudo-complex General Relativity

Abstract

Motivated by possible observations of the black hole candidate in the center of our galaxy and the galaxy M87, ray-tracing methods are applied to both standard General Relativity (GR) and a recently proposed extension, the pseudo-complex General Relativity (pc-GR). The correction terms due to the investigated pc-GR model lead to slower orbital motions close to massive objects. Also the concept of an innermost stable circular orbit (ISCO) is modified for the pc-GR model, allowing particles to get closer to the central object for most values of the spin parameter $a$ than in GR. Thus, the accretion disk, surrounding a massive object, is brighter in pc-GR than in GR. Iron K$\alpha$ emission line profiles are also calculated as those are good observables for regions of strong gravity. Differences between the two theories are pointed out.

revised version

References in corpus (5)

• A Periodic Table for Black Hole Orbits
• K$\alpha$ iron line profile from accretion disks around regular and singular exotic compact objects
• Pseudo-complex General Relativity
• Experimental tests of pseudo-complex General Relativity
• Pseudo-Complex General Relativity: Schwarzschild, Reissner-Nordström and Kerr Solutions

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