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arXiv · 1312.1170

Ray-tracing in pseudo-complex General Relativity

T. Schönenbach·G. Caspar·P. O. Hess·T. Boller·A. Müller·M. Schäfer·W. Greiner
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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$α$ emission line profiles are also calculated as those are good observables for regions of strong gravity. Differences between the two theories are pointed out.

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T. Schönenbach, G. Caspar, P. O. Hess, T. Boller, A. Müller, M. Schäfer, W. Greiner. 2014-04-29. Ray-tracing in pseudo-complex General Relativity. https://doi.org/10.1093/mnras%2Fstu833

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